# A Suzaku survey of Fe K lines in Seyfert 1 active galactic nuclei

R. Patrick, A., N. Reeves, J., Delphine Porquet, G. Markowitz, A., V. Braito,, P. Lobban, A.

► To cite this version:

R. Patrick, A., N. Reeves, J., Delphine Porquet, G. Markowitz, A., V. Braito,, et al.. A Suzaku survey of Fe K lines in Seyfert 1 active galactic nuclei. Monthly Notices of the Royal Astronomical Society, 2012, 426 (3), pp.2522-2565. 10.1111/j.1365-2966.2012.21868.x. hal-02327624

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# A Suzaku survey of Fe K lines in Seyfert 1 active galactic nuclei

A. R. Patrick,¹★ J. N. Reeves,¹,² D. Porquet,³ A. G. Markowitz,⁴,⁵† V. Braito⁶,⁷ and A. P. Lobban¹,⁶

¹Astrophysics Group, School of Physical Sciences, Keele University, Keele, Staffordshire ST5 5BG

²Department of Physics, University of Maryland Baltimore County, MD 21250, USA

³Observatoire astronomique de Strasbourg, Université de Strasbourg, CNRS, UMR 7550, 11 rue de l'Université, F-67000 Strasbourg, France

⁴Dr Karl Remeis-Sternwarte and Erlangen Centre for Astroparticle Physics, Frederic-Alexander Universität Erlangen-Nürnberg, 7 Sternwartstrasse, 96049 Bamberg, Germany

⁵Center for Astrophysics and Space Sciences, University of California, San Diego, M.C. 0424, La Jolla, CA 92093, USA

⁶X-Ray Astronomy Observational Group, Department of Physics and Astronomy, Leicester University, Leicester LE1 7RH

⁷INAF – Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy

Accepted 2012 August 5. Received 2012 August 2; in original form 2012 April 12

## ABSTRACT

We construct full broad-band models in an analysis of Suzaku observations of nearby Seyfert 1 active galactic nuclei (AGN) ($z \le 0.2$) with exposures >50 ks and with greater than 30 000 counts in order to study their iron line profiles. This results in a sample of 46 objects and 84 observations. After a full modelling of the broad-band Suzaku and Swift-Burst Alert Telescope data (0.6–100 keV), we find complex warm absorption is present in 59 per cent of the objects in this sample which has a significant bearing upon the derived Fe K region parameters. Meanwhile 35 per cent of the 46 objects require some degree of high column density partial coverer in order to fully model the hard X-ray spectrum. We also find that a large number of the objects in the sample (22 per cent) require high velocity, high ionization outflows in the Fe K region resulting from Fe xxv and Fe xxvi. A further four AGN feature highly ionized Fe K absorbers consistent with zero outflow velocity, making a total of 14/46 (30 per cent) AGN in this sample showing evidence for statistically significant absorption in the Fe K region.

Narrow Fe $K\alpha$ emission from distant material at 6.4 keV is found to be almost ubiquitous in these AGN. Examining the 6–7 keV Fe K region we note that narrow emission lines originating from Fe xxv at 6.63–6.70 keV and from Fe xxvi at 6.97 keV are present in 52 and 39 per cent of objects, respectively.

Our results suggest statistically significant relativistic Fe $K\alpha$ emission is detected in 23 of 46 objects (50 per cent) at >99.5 per cent confidence, measuring an average emissivity index of $q = 2.4 \pm 0.1$ and equivalent width (EW) $= 96 \pm 10$ eV using the RELLINE model. When parametrized with a Gaussian we find an average line energy of $6.32 \pm 0.04$ keV, $\sigma_{width} = 0.470 \pm 0.05$ keV and EW $= 97 \pm 19$ eV. Where we can place constraints upon the black hole spin parameter $a$, we do not require a maximally spinning black hole in all cases.

**Key words:** black hole physics – galaxies: active – galaxies: Seyfert – X-rays: galaxies.

## 1 INTRODUCTION

The analysis of the X-ray spectra of active galactic nuclei (AGN) can reveal information regarding the inner regions of the accretion disc, the AGN environment as a whole and subsequently the supermassive black hole (SMBH) at its heart. It was suggested by Fabian et al. (1989) that emission occurring from the very in-

ner regions of the accretion disc may be visible and subsequently broadened by Doppler motions and relativistic effects. The majority of AGN spectra show narrow line emission from neutral iron at 6.4 keV (Fe $K\alpha$) likely originating from distant material, e.g. the torus or the outer regions of the accretion disc (Krolik & Kallman 1987; Nandra 2006), particularly strong due to the high abundance and fluorescent yield of iron. If Fe $K\alpha$ emission additionally arises from material close to the central SMBH, it will become relativistically broadened (Fabian et al. 1989; Laor 1991), producing both blue and red wings to the traditionally narrow line profile.

<footnote>*E-mail: a.patrick@keele.ac.uk</footnote>

<footnote>†Alexander von Humboldt Fellow.</footnote>
In some AGN spectra this relativistic Fe Kα emission may be strong enough to be observed allowing its shape and strength measured using disc-line emission models such as LAOR, KYRLINE, KERDIDISK and RELLINE (Laor 1991; Dovčiak, Karas & Yaqoob 2004; Brenneman & Reynolds 2006; Dauser et al. 2010). The application of these models allows properties such as the inclination and emissivity index of the disc to be measured in addition to the typical inner radius of emission and in some cases the spin of the central SMBH (Nandra et al. 2007; Patrick et al. 2011a). Gaining information regarding the distribution of SMBH spins is an essential tool in aiding our understanding of galaxy evolution and distinguishing between models such as prolonged or chaotic accretion and also the effect of mergers upon the SMBH spin (Hughes & Blandford 2003; Volonteri et al. 2005; King & Pringle 2007; Rezzolla et al. 2008). A spin distribution skewed towards higher values (a ~ 0.998) would suggest prolonged accretion, whereas low SMBH spin (a ~ 0) would indicate chaotic accretion models are more appropriate. In addition to this, the magnetic extraction of black hole (BH) rotational energy through the Blandford–Znajek effect (Blandford & Znajek 1977) could cause a reduction in the spin (i.e. towards zero) of the SMBH in some AGN (Berti & Volonteri 2008).

Recent publications have made steps towards making spin estimates of SMBHs in a variety of AGN, including those which feature low levels of intrinsic absorption thereby offering the simplest spectrum to analyse, avoiding complications regarding the degree of spectral curvature introduced with warm absorbing zones (Miniutti et al. 2009; Schmoll et al. 2009; Emmanoulopoulos et al. 2011; Patrick et al. 2011a). More complex AGN spectra have also been analysed and revealed further spin estimates e.g. MCG–06–30–15 (Miniutti et al. 2007; Patrick et al. 2011b), Mrk 79 (Gallo et al. 2011) and NGC 3783 (Brenneman et al. 2011; Patrick et al. 2011b). However, as discussed in Patrick et al. (2011a), the estimated SMBH spin is highly model-dependent and strongly related to the treatment of features such as the soft excess or any intrinsic absorbing zones. Assuming a Comptonization origin of the soft excess results in a range of low to intermediate spins, whereas using a high degree of relativistic blurring to smooth the discrete soft emission lines into a continuum typically forces the spin to near-maximal values requires very high disc emissivities.

This paper includes a sample of AGN from the public *Suzaku* archive of all observations of Seyfert 1 AGN with total exposures >50 ks and more than 30 000 counts in order to increase the likelihood of detection and broadened emission from the inner regions if it is present. *Suzaku* is the ideal instrument with which to do this work since it allows us to gather both soft and hard X-ray data simultaneously using the X-ray Imaging Spectrometer (XIS; Koyama et al. 2007) and Hard X-ray Detector (HXD; Takahashi et al. 2007) detectors which, when combined with further non-simultaneous hard X-ray data from Swift-Burst Alert Telescope (Swift-BAT), give a broad energy bandpass of 0.6–100.0 keV. The crucial difference being that we can obtain data regarding the strength of the Compton reflection hump at ~30 keV (George & Fabian 1991), which is beyond the capabilities of other current X-ray observatories. Only with hard X-ray data can the strength of the reflection component be appropriately constrained and hence its contribution to the Fe K region assessed prior to attempting to determine broadening in the Fe K region and eventually estimates upon SMBH spin.

This is the final paper in a series of three in which a methodical and relatively uniform approach has been taken in an attempt to constrain accretion disc properties and SMBH spin from the Fe K regions from an analysis of the X-ray spectra of Seyfert 1 AGN. In Patrick et al. (2011a) a small sample of six ‘bare’

Seyfert 1 AGN (i.e. those featuring low intrinsic absorption: Ark 120, Fairall 9, MCG–02–14–009, Mrk 335, NGC 7469 and SWIFT J2127.4+5654) was analysed, finding that narrow ionized emission lines such as Fe XXVI are relatively common (4/6 objects), while the emissivity index of the accretion disc indicated that no strongly centrally concentrated emission was required to model any relativistic broadening in the Fe K region with an average of $q \sim 2.3 \pm 0.2$.

Patrick et al. (2011b) undertook an analysis of high-quality, long-exposure (>200 ks) observations of Seyfert 1 AGN with *Suzaku* (Fairall 9, MCG–06–30–15, NGC 3516, NGC 3783 and NGC 4051), making use of the full 0.6–100.0 keV bandpass in order to fully account for any warm absorber component to give the best possible opportunity to make estimates upon SMBH spin, also finding a low to moderate average emissivity index of $q \sim 2.8 \pm 0.2$. Other authors have also made some progress towards making spin estimates on Seyfert 1 AGN, e.g. Miniutti et al. (2009), Schmoll et al. (2009), Nardini et al. (2011), Gallo et al. (2011), Emmanoulopoulos et al. (2011) and Brenneman et al. (2011).

The main aim of this paper is to assess the properties and total percentage of AGN which have been observed with *Suzaku* that show evidence for broadened line emission in the Fe K region from the inner regions of the accretion disc resulting from an analysis of the broad-band X-ray spectrum. In this paper we expand our broad-band spectral analysis with *Suzaku* to all the currently archived type 1–1.9 AGN, which have at least a 50-ks total exposure and 30 000 XIS band counts, sufficient for a broad-band spectral analysis. This enables us to measure the iron line and reflection properties of a more substantial sample of 46 type 1 AGN, allowing the overall properties of the iron line and accretion disc to be investigated. We also aim to investigate *Suzaku*'s view of ionized emission and absorption lines in the Fe K region and the occurrence of warm absorbers, highly ionized absorbers and partially covering absorbers and the subsequent effects upon the AGN X-ray spectrum.

# 2 OBSERVATIONS AND DATA REDUCTION

## 2.1 Observations and sample selection

The objects included within this sample are listed in Table 1 and are all the Seyfert 1–1.9 AGN with exposures >50 ks and greater than 30 000 0.6–10.0 keV counts which have been observed with *Suzaku* with data publicly available in the *Suzaku* data archive<fnref n="1" /> as of 2011 September. We also include data from some type 1 radio-loud (BLRGs – non-blazar) AGN, provided they fit the above exposure and count criteria. High-energy X-ray data from *Swift-BAT* from the 58-month BAT catalogue are also used in addition to that obtained from the HXD detector on-board *Suzaku* (but allowing the relative cross-normalization to vary), therefore the total energy range covered is 0.6–100.0 keV. Details of the observations included are listed in Table B1.

In some instances, objects may have been observed on numerous occasions, provided that there is little variation between the data sets they are combined and a single analysis is performed. If the observations do indeed vary, a separate analysis is performed on each data set, although with similar model components and inferred geometries where possible, e.g. the inclination angle of the accretion disc would be linked between observations.

<footnote n="1">¹ http://heasarc.gsfc.nasa.gov/</footnote>
<table><caption>**Table 1.** The *Suzaku* Seyfert sample.</caption><thead><tr><th>Object</th><th>RA (J2000)</th><th>Dec. (J2000)</th><th>Redshift</th><th>N<sub>H</sub> (Gal) (×10<sup>22</sup> cm<sup>-2</sup>)</th></tr></thead><tbody><tr><td>1H 0419-577</td><td>04 26 00.8</td><td>-57 12 00.4</td><td>0.1040</td><td>0.0126</td></tr><tr><td>3C 111</td><td>04 18 21.3</td><td>+38 01 35.8</td><td>0.0485</td><td>0.2910</td></tr><tr><td>3C 120</td><td>04 33 11.1</td><td>+05 21 15.6</td><td>0.0330</td><td>0.1060</td></tr><tr><td>3C 382</td><td>18 35 03.4</td><td>+32 41 46.8</td><td>0.0579</td><td>0.0714</td></tr><tr><td>3C 390.3</td><td>18 42 09.0</td><td>+79 46 17.1</td><td>0.0561</td><td>0.0347</td></tr><tr><td>3C 445</td><td>22 23 49.5</td><td>-02 06 12.9</td><td>0.0559</td><td>0.0559</td></tr><tr><td>4C 74.26</td><td>20 42 37.3</td><td>+75 08 02.4</td><td>0.1040</td><td>0.1160</td></tr><tr><td>Ark 120</td><td>05 16 11.4</td><td>-00 08 59.4</td><td>0.0327</td><td>0.0978</td></tr><tr><td>Ark 564</td><td>22 42 39.3</td><td>+29 43 31.3</td><td>0.0247</td><td>0.0534</td></tr><tr><td>Fairall 9</td><td>01 23 45.8</td><td>-58 48 20.5</td><td>0.0470</td><td>0.0316</td></tr><tr><td>IC 4329A</td><td>13 49 19.3</td><td>-30 18 34.0</td><td>0.0161</td><td>0.0461</td></tr><tr><td>IRAS 13224-3809</td><td>13 25 19.4</td><td>-38 24 52.7</td><td>0.0658</td><td>0.0534</td></tr><tr><td>MCG-02-14-009</td><td>05 16 21.2</td><td>-10 33 41.4</td><td>0.0285</td><td>0.0924</td></tr><tr><td>MCG-02-58-22</td><td>23 04 43.65</td><td>-08 41 08.6</td><td>0.0649</td><td>0.0291</td></tr><tr><td>MCG-05-23-16</td><td>09 47 40.2</td><td>-30 56 55.9</td><td>0.0085</td><td>0.0870</td></tr><tr><td>MCG-06-30-15</td><td>13 35 53.8</td><td>-34 17 44.1</td><td>0.0077</td><td>0.0392</td></tr><tr><td>MCG+8-11-11</td><td>05 54 53.6</td><td>+46 26 21.6</td><td>0.0205</td><td>0.1840</td></tr><tr><td>MR 2251-178</td><td>22 54 05.8</td><td>-17 34 55.0</td><td>0.0640</td><td>0.0640</td></tr><tr><td>Mrk 79</td><td>07 42 32.8</td><td>+49 48 34.8</td><td>0.0222</td><td>0.0527</td></tr><tr><td>Mrk 110</td><td>09 25 12.9</td><td>+52 17 10.5</td><td>0.0353</td><td>0.0130</td></tr><tr><td>Mrk 205</td><td>12 21 44.0</td><td>+75 18 38.5</td><td>0.0708</td><td>0.0280</td></tr><tr><td>Mrk 279</td><td>13 53 03.5</td><td>+69 18 29.6</td><td>0.0305</td><td>0.0152</td></tr><tr><td>Mrk 335</td><td>00 06 19.5</td><td>+20 12 10.5</td><td>0.0258</td><td>0.0356</td></tr><tr><td>Mrk 359</td><td>01 27 32.5</td><td>+19 10 43.8</td><td>0.0174</td><td>0.0426</td></tr><tr><td>Mrk 509</td><td>20 44 09.7</td><td>-10 43 24.5</td><td>0.0344</td><td>0.0344</td></tr><tr><td>Mrk 766</td><td>12 18 26.5</td><td>+29 48 46.3</td><td>0.0129</td><td>0.0178</td></tr><tr><td>Mrk 841</td><td>15 04 01.2</td><td>+10 26 16.2</td><td>0.0364</td><td>0.0222</td></tr><tr><td>NGC 1365</td><td>03 33 36.4</td><td>-36 08 25.5</td><td>0.0055</td><td>0.0134</td></tr><tr><td>NGC 2992</td><td>09 45 42.1</td><td>-14 19 35.0</td><td>0.0077</td><td>0.0487</td></tr><tr><td>NGC 3147</td><td>10 16 53.7</td><td>+73 24 02.7</td><td>0.0093</td><td>0.0285</td></tr><tr><td>NGC 3227</td><td>10 23 30.6</td><td>+19 51 54.2</td><td>0.0039</td><td>0.0199</td></tr><tr><td>NGC 3516</td><td>11 06 47.5</td><td>+72 34 06.9</td><td>0.0088</td><td>0.0345</td></tr><tr><td>NGC 3783</td><td>11 39 01.7</td><td>-37 44 18.9</td><td>0.0097</td><td>0.0991</td></tr><tr><td>NGC 4051</td><td>12 03 09.6</td><td>+44 31 52.8</td><td>0.0023</td><td>0.0115</td></tr><tr><td>NGC 4151</td><td>12 10 32.6</td><td>+39 24 20.6</td><td>0.0033</td><td>0.0230</td></tr><tr><td>NGC 4593</td><td>12 39 39.4</td><td>-05 20 39.3</td><td>0.0090</td><td>0.0189</td></tr><tr><td>NGC 5506</td><td>14 13 14.9</td><td>-03 12 27.3</td><td>0.0062</td><td>0.0408</td></tr><tr><td>NGC 5548</td><td>14 17 59.5</td><td>+25 08 12.4</td><td>0.0172</td><td>0.0155</td></tr><tr><td>NGC 7213</td><td>22 09 16.3</td><td>-47 09 59.8</td><td>0.0058</td><td>0.0106</td></tr><tr><td>NGC 7314</td><td>22 35 46.2</td><td>-26 03 01.7</td><td>0.0048</td><td>0.0150</td></tr><tr><td>NGC 7469</td><td>23 03 15.6</td><td>+08 52 26.4</td><td>0.0163</td><td>0.0445</td></tr><tr><td>PDS 456</td><td>17 28 19.8</td><td>-14 15 55.9</td><td>0.1840</td><td>0.1960</td></tr><tr><td>PG 1211+143</td><td>12 14 17.7</td><td>+14 03 12.6</td><td>0.0809</td><td>0.0274</td></tr><tr><td>RBS 1124</td><td>12 31 36.4</td><td>+70 44 14.1</td><td>0.2080</td><td>0.0152</td></tr><tr><td>SWIFT J2127.4+5654</td><td>21 27 45.0</td><td>+56 56 39.7</td><td>0.0144</td><td>0.7650</td></tr><tr><td>TON S180</td><td>00 57 19.9</td><td>-22 22 59.1</td><td>0.0620</td><td>0.0136</td></tr></tbody></table>

## 2.2 Data reduction

The *Suzaku* data in this paper were reduced using version 6.10 of the HEASOFT data reduction and analysis package. The XIS source spectra were extracted using 3.0-arcmin circular regions centred on the source. Background spectra were also extracted using 3.0-arcmin circular regions, this time centred on a region of the CCD not featuring any of the source or Fe 55 calibration regions. Only data from the front-illuminated XIS 0, 2 and 3 detectors were used due to their greater sensitivity at Fe K energies; however, data from the back-illuminated XIS 1 remain consistent with the front-illuminated detectors. Observations since 2006 November, however, do not include data from XIS 2 as it is no longer operational.

Objects which have been observed on multiple occasions but where the X-ray spectra (or spectral shape) does not appear to have

varied by a significant amount (e.g. other than simple changes in power-law normalization) are combined into a single data file and then a suitable model is fitted to the data. This is the case for IC 4329A, MCG-06-30-15, Mrk 509, Mrk 841, NGC 2992 and NGC 5548. However, if there are discernible differences between multiple observations of the same object (e.g. differing spectra shapes or changes in absorption), these data sets are analysed separately while retaining as many similar model components as possible. Such an analysis is performed for Fairall 9, NGC 1365, NGC 3227, NGC 3516, NGC 3783 and NGC 4051. Both of the 2006 observations of NGC 5506 are combined into a single spectrum, while the 2007 observation is kept separate. Similarly, the later three observations of 3C 120 are combined, while the first observation (OBSID: 700001010, see Table B1) is analysed separately. MCG-06-30-15 was observed on three occasions in 2006 January; this paper makes
use of all the three observations and the time-averaged spectrum is used in the main analysis. Analysis of the individual observations yields Fe K line profiles which were consistent within errors and as such all three of the 2006 January observations have been co-added. Systematic errors are not included in data sets other than NGC 1365 in which systematic errors are set at 2 per cent.

The HEASOFT tool XISRMFGEN was used to generate the XIS redistribution matrix files, and the ancillary response files were generated using XISSIMARFGEN. The data from each of the front-illuminated XIS detectors were then co-added using MATHPHA, ADDRMF and ADDARF in order to increase signal-to-noise ratio (S/N). We ignore all XIS data below 0.6 keV, above 10.0 keV and between 1.7 and 2.0 keV due to calibration uncertainties of the detectors around the Si K edge. Some of the most recent observations with Suzaku (2011 onwards) show evidence for contamination on the CCD of XIS 0 which primarily affects the soft X-ray energies resulting in a divergence of XIS 0 with XIS 3 below 1 keV. This is notable in the two observations of Fairall 9; both XIS 0 and XIS 3 are consistent in the 2007 observation; however, the 2010 observation displays a notable difference between XIS 0 and XIS 3 (see Fig. 1). In this analysis, we do not co-add XIS 0 and XIS 3 for the contaminated Fairall 9 observation,

<figure><img src="image_2.png" /><figcaption>**Figure 1.** Ratio plots of 0.6–1.0 keV of XIS 0 (red) and XIS 3 (black) for the 2007 (upper panel) and 2010 (lower panel) observations of Fairall 9. These show the contamination which has recently affected XIS 0 at soft X-ray energies causing a divergence with XIS 3; note that this is not apparent in the first observation. The soft X-ray spectrum was modelled with a basic (POWERLAW+COMPTT)*WABS model.</figcaption></figure>

<figure><img src="image_3.png" /><figcaption>**Figure 2.** Ratio plot of the 4–9 keV Fe K regions of XIS 0 (red) and XIS 3 (black) for the 2010 observation of Fairall 9, indicating that while contamination has a significant effect at soft X-ray energies, the Fe K region remains entirely consistent between XIS 0 and XIS 3.</figcaption></figure>

instead preferring to include them as separate data sets although limiting XIS 0 to > 1.0 keV, thus retaining some of the sensitivity at Fe K energies. Both detectors, however, remain consistent at Fe K energies; see Fig. 2.

Spectra from the HXD were extracted from the cleaned HXD/PIN event files and subsequently corrected for instrument dead time using the tool HXDDTCOR. The tuned HXD/PIN non-X-ray background (NXB) event files were used for background subtraction (Fukazawa et al. 2009) and generated with 10 times the actual background rate in order to reduce photon noise, also with identical good time intervals as used in the source events. A simulated cosmic X-ray background was also produced for each observation using XSPEC V 12.6.0q with a spectral form identical to that used in Gruber et al. (1999); this was then added to the corrected NXB to form a single background file for each observation. The appropriate response and flat-field files were used from the Suzaku CALDB suitable for the respective epochs of each observation. HXD data are used over the 15.0–60.0 keV range along with the appropriate PIN/XIS-FI cross-normalization according to the epoch and nominal pointing position.<fnref n="2" />

While the BAT data from Swift are not necessarily simultaneous with the Suzaku observations and are of relatively low statistical weight, we find throughout the paper that the BAT spectral indices are consistent with those obtained from the XIS and HXD/PIN data. That is, due to variability of the reflection fraction over time-scales of years the spectral shape may vary and hence may not be equivalent to the spectral shape of the hard X-rays obtained with Suzaku. However, removing the BAT data and refitting still yield the original photon index Γ as well as the other spectral parameters and there appears to be little evidence that the spectral shape >15 keV varies over the time-scales considered here. It is therefore appropriate to consider that there is a simple change in the normalization of the hard X-ray component (as accounted for by the cross-normalization between XIS and BAT being allowed to vary within the models) and the inclusion of BAT data from Swift serves to improve our view of the X-ray spectral shape above 10 keV. The BAT data therefore improve the accuracy to which we can estimate the power-law continuum and the reflection component.

<footnote n="2">² http://heasarc.gsfc.nasa.gov/docs/suzaku/analysis/watchout.html</footnote>
# 3 ANALYSIS AND RESULTS

Spectral analysis and model fitting are performed from within `XSPEC` v 12.6.0q (Arnaud 1996); all models are modified by Galactic absorption which is accounted for by the `WABS` multiplicative model (Morrison & McCammon 1983). The respective Galactic column densities were obtained using the `NH FTOOL` for each source giving the weighted average $N_H$ value of the LAB Survey of Galactic H I (Kalberla et al. 2005), using abundances from Anders & Grevesse (1989). Data are fitted over the full 0.6–100.0 keV range available, excluding those regions affected by the uncertainties in the XIS calibration mentioned above. The $\chi^2$ minimization technique is used throughout, all errors are quoted at the 90 per cent confidence level ($\Delta\chi^2 = 2.71$ for one interesting parameter) and include statistical and not instrumental systematic errors. Where the significance of components is quoted in terms of $\Delta\chi^2$, the component in question has been removed from the model and the data refitted to ensure that the order in which components are added to the model does not affect the quoted statistical significance. Throughout this paper, a positive $\Delta\chi^2$ corresponds to a poorer fit, whereas a negative $\Delta\chi^2$ corresponds to an improvement in the fit.

## 3.1 Spectral models

The data used in this paper are selected such that there are a sufficient number of counts for detailed spectral analysis to be conducted. The wide 0.6–100.0 keV energy bandpass as used in this sample means that a full treatment must be given to all the main components of the X-ray spectrum of these Seyfert 1 AGN, namely the soft excess, Compton reflection, Galactic absorption, warm absorbers and any highly ionized outflows or relativistic broadening which may be present. In order to model the X-ray spectra in this sample as consistently and uniformly as possible, we construct models following the criteria in the following sections.

Model components are added according the residuals in the data and the statistical requirement of such a component. For example, a model to account for the soft excess is considered to be required, provided that its inclusion exceeds the 90 per cent confidence level according to $\Delta\chi^2$ given the appropriate number of free parameters. For example, an `XSTAR` grid typically has two: column density and ionization parameter, although some objects may require a third due to an outflow velocity.

### 3.1.1 Modelling of the soft excess

A number of AGN spectra show an excess over a simple `POWERLAW` at lower X-ray energies, typically <2.0 keV; this relatively common feature has been termed the ‘soft excess’. The origin of the soft excess is as yet unknown; however, there are a number of different interpretations and methods with which to model it. Perhaps the most basic method of modelling the soft excess is as a blackbody to replicate direct thermal emission from successive annuli of the accretion disc (Malkan & Sargent 1982). The inferred constant temperature of the soft-excess component (which scales with $M_{BH}^{-1/4}$) is in disagreement with the typical accretion disc properties of a SMBH and is arguably more suitable for an intermediate-mass BH (Gierliński & Done 2004).

A variation upon this concept is that the soft excess is produced by the Compton upscattering of extreme-ultraviolet seed photons from the disc in a hot plasma or corona lying above the disc. For example, the `COMPTT` model (Titarchuk 1994) allows for a large variation in photon seed temperature while still producing a relatively constant

output photon temperature as is required by many of the observed soft excesses in AGN. This method has been successful in modelling the soft excess of a large number of AGN, including a sample of PG quasars (Porquet et al. 2004) and in Mrk 509 by Mehdipour et al. (2011). This interpretation of the soft excess is also used throughout this paper, consistent with the method in Patrick et al. (2011a,b); similar results can also be obtained with a second steep `POWERLAW` component.

The above methods assume a smooth shape to account for the soft excess; however alternatives have been suggested, e.g. an atomic origin (Brenneman & Reynolds 2006). Soft X-ray emission lines emitted from regions close to the central SMBH are relativistically blurred and broadened, much in the same way as the often observed broad 6.4-keV Fe Kα emission line and its red wing. A series of discrete emission-line features are then relativistically blurred to such an extent that they merge to form a smooth continuum (Ross, Fabian & Ballantyne 2002). A number of AGN have been modelled in this fashion, e.g. Ark 120, Fairall 9, Mrk 335 and RBS 1124 (Schmoll et al. 2009; Miniutti et al. 2010; Nardini et al. 2011; Patrick et al. 2011a), although a significant amount of relativistic blurring is required to smooth the characteristically narrow features into a broad continuum forces the accretion disc emissivity index to high values ($q \gtrsim 4.5$) and SMBH spin towards near maximal ($a \sim 0.998$). Indeed Schmoll et al. (2009) note that ignoring the XIS data below 2 keV (to avoid fitting the soft excess) relaxes the spin constraint to low values. These parameters are often at odds with those similarly derived from the asymmetric line profile from the Fe K region, for example Miniutti et al. (2010) find $q = 4.1_{-0.9}^{+5.3}$ and $a \ge 0.6$ in RBS 1124 while the authors note that there is no evidence for a strong broad line in the Fe K region. However, given the assumption that the material responsible for both the soft emission lines and Fe Kα emission is located in the same region, it is logical to assume that estimated accretion disc and SMBH parameters should be consistent (Patrick et al. 2011a).

Note that relativistic blurring of the reflection component at soft X-ray energies can still contribute towards the soft excess; however, the soft X-ray flux from relativistically blurred emission of the inner regions is unlikely to prove particularly strong in comparison to the flux from the Comptonization component due to any residuals in the Fe K region driving the fit with the majority of the soft X-ray flux already accounted for with the `COMPTT` model. Therefore, if the Fe K line is to be used as a diagnostic for determining accretion disc parameters and constraining SMBH spin, the treatment of the soft excess has a significant role to play in ensuring that it is not driving the fit if blurred reflection models are used in the fitting process. As our aim is to parametrize the properties of the disc and reflection based on the Fe K line profile, independent of the nature of the soft excess, we retain this approach of the Comptonization origin of the soft excess here.

### 3.1.2 Compton reflection and emission lines

As the narrow Fe Kα line is ubiquitous in virtually all these AGN, an `unblurred` `REFLIONX` (Ross & Fabian 2005) component measured down to an ionization parameter of $\xi = 1$ and additional narrow fluorescent emission lines representative of reflection off distant material (e.g. the torus or outer regions of the accretion disc) are included in all AGN spectra showing evidence for a hard excess. Previous studies of the iron line regions in Seyfert AGN by Bianchi et al. (2004), Nandra et al. (2007) and Patrick et al. (2011a,b) also suggest that ionized species of iron are relatively common at
energies of 6.7 and 6.97 keV for Fe XXV and Fe XXVI, respectively. Neutral narrow Fe Kα and the accompanying Fe Kβ emission at 6.4 and 7.056 keV respectively are ubiquitous in AGN spectra (Nandra et al. 2007).

As stated above, in this paper we use the REFLIONX model to account for the distant near-neutral reflection continuum with the input photon index Γ tied to that of the intrinsic POWERLAW. Although soft emission lines are included in REFLIONX, these are also added on an ad hoc basis when required and as such are modelled using narrow Gaussians of fixed width σ = 0.01 keV, e.g. O VIII or Ne IX emission from distant photoionized gas e.g. the broad-line region (BLR) or narrow-line region (NLR). Fe Kβ emission at 7.056 keV with flux F<sub>Kβ</sub> = 0.13 × F<sub>Kα</sub> is not included self-consistently in REFLIONX, which is therefore modelled using a narrow Gaussian of fixed width σ = 0.01 keV and with flux fixed at the value obtained during an initial parametrization of the Fe K region and the narrow Fe Kα flux when modelled with a Gaussian. Ionized lines in the Fe K region (such as Fe XXV at ~6.63–6.7 keV and Fe XXVI at 6.97 keV) are accounted for with narrow Gaussians (σ = 0.01 keV) if and when required, although in some circumstances these can be indistinguishable from the blue wing of a relativistically broadened Fe Kα line profile.

While the iron abundance Z<sub>Fe</sub> is left free to vary, in some AGN the strength of the narrow Fe Kα core may force Z<sub>Fe</sub> to unfeasibly high values (e.g. Z<sub>Fe</sub> ≳ 3) while improperly modelling the hard X-ray reflection spectrum due to the greater number of counts in the 5–6 keV region. To avoid this scenario, we fix Z<sub>Fe</sub> at solar abundance and add an additional narrow Gaussian of fixed width (σ = 0.01 keV, to prevent interference with any broad component from the disc) at 6.4 keV to model the Fe Kα core while maintaining a good fit to the HXD and BAT data. Rather than simply being an ad hoc solution, this could be representative of Fe Kα emission additionally arising from Compton-thin matter such as the BLR or NLR as well as e.g. scattering off a distant Compton-thick torus.

### 3.1.3 Warm absorption

The X-ray spectra of many AGN feature one or more zones of warm absorbing gas, while primarily affecting the spectrum at soft X-ray energies, with higher column densities (e.g. >10<sup>22</sup> cm<sup>-2</sup>) it can add subtle curvature above 2.5 keV. Previous studies (e.g. Miniutti et al. 2007; Nandra et al. 2007) restrict their analysis to 2.5–10.0 keV to avoid complications with the warm absorber, instead choosing to focus in upon the Fe K region. However, as found in Reeves et al. (2004), Turner et al. (2005), Miller, Turner & Reeves (2009) and Patrick et al. (2011b), effects of the warm absorber extend even to the Fe K region, contributing significantly to the strength of the observed red wing below 6.4 keV. For example, in MCG–06-30-15. Miniutti et al. (2007) model the time-averaged 2006 January spectra without absorption, resulting in an apparent strong broad Fe Kα line and near-maximal SMBH spin; while a full treatment of the warm absorber appears to reduce the strength of the broad component and subsequently BH spin to more intermediate values (Zycki et al. 2010; Patrick et al. 2011b).

To model the soft X-ray warm absorber components in this paper, we use an XSTAR (Kallman et al. 2004) generated grid illuminated by an X-ray photon index of Γ = 2.0, in agreement with the mean values found in radio-quiet type I AGN (Scott et al. 2011). The abundances are fixed at solar values (except Ni, which was set to zero), where XSTAR uses the values of Grevesse & Sauval (1998). The turbulent velocity is set to 100 km s<sup>-1</sup>. The grid is well suited to

accounting for a variety of absorption zones due to its wide range in column density (5 × 10<sup>18</sup> cm<sup>-2</sup> < N<sub>H</sub> < 5 × 10<sup>24</sup> cm<sup>-2</sup>, in steps of ΔN<sub>H</sub> = 10<sup>19</sup> cm<sup>-2</sup>) and ionization parameter [0 < log ξ < 5, with grid steps Δ(log ξ) = 0.5]. An electron density of n<sub>e</sub> = 10<sup>10</sup> cm<sup>-3</sup> is assumed, although the data are largely insensitive to the density at CCD resolution. The computed XSTAR spectra were generated over the energy range from 0.05 to 120 keV, so they are suited to broad-band spectra, especially at hard X-ray energies.

During the fitting process absorption zones are added as required, in some objects more than one zone may be statistically required and in exceptional circumstances a grid with a higher turbulent velocity may be required to model highly ionized absorption in the Fe K region (see below), as at low turbulences the Fe K absorption can become easily saturated. Absorption zones are added until a good overall fit is found to the data and there are no clear residuals remaining in the soft X-ray spectrum.

### 3.1.4 Highly ionized absorption

Further to typical warm absorption, highly ionized absorbing zones of gas (where present) also play an important role in the Fe K region and in the determination of the measured line parameters and strength of the observed red wing (Reeves et al. 2004; Turner et al. 2005). Absorption lines indicative of such zones are fairly common in X-ray spectra of AGN, e.g. 1s–2p resonance lines from Fe XXV and/or Fe XXVI at their rest-frame energies, i.e. 6.7 and 6.97 keV respectively, although there is evidence for blueshifted absorption lines in many AGN (Braito et al. 2007; Tombesi et al. 2010a; Lobban et al. 2011).

In the event that absorption features in the Fe K region are found, which are not adequately modelled by the above low-turbulence grid, then these are accounted for using a model representative of a highly ionized absorption zone. We use an XSTAR generated grid with a turbulent velocity of 1000 km s<sup>-1</sup>, with an input X-ray photon index of Γ = 2.0 and using the input spectral energy distribution from Tombesi et al. (2011). This grid covers a range in column density and ionization parameter of 1 × 10<sup>20</sup> < N<sub>H</sub> < 1 × 10<sup>24</sup> cm<sup>-2</sup> (in steps ΔN<sub>H</sub> = 6 × 10<sup>19</sup> cm<sup>-2</sup>) and 0 < log ξ < 6 [with Δ(log ξ) = 0.32], respectively. The electron density assumed is also n<sub>e</sub> = 10<sup>10</sup> cm<sup>-3</sup>.

### 3.1.5 Partial covering

Some models used in the analysis of these AGN use partial covering geometries whereby a fraction of the observed X-rays are absorbed by a surrounding gas in the line of sight (in addition to typical fully covering absorbers) as described in Section 3.1.3, while some fraction of the continuum ‘leaks’ or scatters through and is unattenuated by the partially covering material (e.g. Miller, Turner & Reeves 2008). The partial coverer used here takes the form of (POWERLAW + XSTAR*POWERLAW) with the photon index of both the power-law components tied and normalizations of both power laws free to vary. The parameters of the warm absorber (ionization and column density) are also allowed to vary. The column density of the partially covering medium can have a significant effect upon the spectrum. For example, high column partial coverers (N<sub>H</sub> ~ 10<sup>24</sup> cm<sup>-2</sup>) predominantly affect the hard X-ray energies and can contribute towards a hard X-ray excess in cases where a hard excess remains (i.e. in addition to REFLIONX). Lower column density partial coverers may greatly affect spectral curvature at lower X-ray energies and in some cases can entirely remove any ‘broad’ residuals in
the Fe K region (Miller et al. 2009). While using a partial coverer in this way provides an alternate explanation for observed curvature or a red wing in the Fe K region, we restrict the analysis to a maximum of one partially covering zone in order to not arbitrarily model away spectral features present in the spectra. The absorption grid used is the same as used to model the warm absorber, with a turbulence of 100 km s⁻¹.

### 3.1.6 Relativistic line emission

The majority of X-ray lines originate from material sufficiently distant to the SMBH (e.g. the ubiquitous narrow 6.4-keV line) such that effects such as relativistic Doppler motions and gravitational redshift have a negligible effect upon the observed spectrum. If, however, emission comes from the very inner regions of the accretion disc, it will of course be subjected to these effects. As discussed above, this is one interpretation for the commonly observed red wing in the Fe K regions of some AGN which may remain after a full modelling of the broad-band spectrum, taking into account warm absorbers which may be present. If an excess remains at ~5–6.4 keV, we initially model this using the relativistic line emission model RELLINE (Dauser et al. 2010). This allows properties such as the emissivity index and inclination of the disc to be measured in addition to placing estimates upon the spin of the central SMBH (or the inner radius of emission). A more comprehensive modelling of the inner regions of the accretion disc would include the accompanying blurred reflection spectrum. For example, a convolution of the RELLINE kernel (i.e. RELCONV; Dauser et al. 2010) with REFLIONX allows relativistic effects to be applied to both the hard and soft X-ray reflection spectrum as well as to the Fe Kα emission line at 6.4 keV; we investigate such an approach in Section 3.4.

## 3.2 Baseline model

The baseline model is intended to model the entire 0.6–100.0 keV spectrum, accounting for features such as the underlying continuum, soft excess, *distant* reflection, and both warm and neutral absorption. With this model we aim to assess the remaining residuals in the Fe K region which may be attributed to relativistic line emission from the inner regions of the accretion disc, i.e. we use a combination of the models and methods outlined in Section 3.1 to form a baseline model which does not include broadened line emission. The baseline model acts as the null hypothesis whereby the X-ray spectrum of these AGN can be described and adequately fitted by emission or reflection from purely distant material. Fig. 3 therefore shows the Fe K regions of these AGN prior to any modelling of broad emission, distant emission lines or highly ionised absorption.

### 3.2.1 Analysis of ‘bare’ Seyfert spectra

As noted in Patrick et al. (2011b) the warm absorber below 2.5 keV has a significant effect upon the X-ray spectrum at higher energies, particularly important when attempting to test for the strength or indeed presence of a relativistically broadened red wing in the Fe K region. Subsequently the broad-band 0.6–100.0 keV analysis conducted here suggests that the majority of Seyfert 1 AGN in this sample show evidence for at least one warm absorber zone or additional neutral absorption over the simple Galactic absorbing column.

Only 11/46 objects in this sample can be considered ‘bare’ in that no absorption (either neutral, warm or partially covering) whatsoever is required: 3C 390.3, Ark 120, Fairall 9, MCG–02-14-009, Mrk 110, Mrk 335, Mrk 359, NGC 3147, NGC 7213, NGC 7469 and RBS 1124. These AGN are therefore straightforward to model, without any complications due to curvature from warm absorbing components, representing the most fiducial of AGN X-ray spectra simply consisting of (POWERLAW+COMPTT+REFLIONX)*WABS. Slightly more complex are those objects which are free from warm absorption; however, requiring an additional neutral absorbing column over and above that from the standard Galactic absorption calculated by the NH FTOOL. This is accounted for by multiplying the typical ‘bare’ AGN model by a single ZPHABS fixed at the redshift of the object with column density free to vary, as used in 6/46 of AGN in the sample: 3C 111, 3C 120, MCG–05-23-16, NGC 2992, NGC 7314 and SWIFT J2127.4+5654. Note that the higher neutral absorption in 3C 111 is likely due to the presence of a giant molecular cloud in the line of sight; see Bania et al. (1991) and Rivers, Markowitz & Rothschild (2011b). MCG–05-23-16 does not require an additional totally covering zone of neutral absorption, instead requiring a neutral ZPHABS geometry whereby only the POWERLAW component is absorbed. Two further AGN (Mrk 205 and PDS 456) require a partial coverer, but not a warm absorber. Hence a total of 19/46 objects in this sample do not indicate the presence of a warm absorbing component.

### 3.2.2 Absorbed Seyfert spectra – fully covering

The remaining objects in the sample (27/46) feature some degree of complex warm absorption, which is modelled with successive zones of a multiplicative XSTAR grid (see Table 2). The majority of these AGN are well modelled using one or more fully covering XSTAR grids with turbulent velocity $v_{\text{turb}} = 100 \text{ km s}^{-1}$ fixed at the redshift of the object (i.e. from Table 1) as described in Section 3.1.3.

Rather using the typical $v_{\text{turb}} = 100 \text{ km s}^{-1}$ XSTAR grid, some AGN in this sample require the use of an XSTAR generated grid with $v_{\text{turb}} = 1000 \text{ km s}^{-1}$ i.e. the turbulent velocity exceeds the local thermal velocity of the absorbing ion, proving to be the dominant factor for absorption line broadening; see Fig. 4. This scenario is required when modelling the soft X-ray absorber in only 3/28 of objects featuring complex absorption: 3C 445, Ark 564 and IC 4329A. IC 4329A requires two low $v_{\text{turb}}$ XSTAR grids in addition to the single high $v_{\text{turb}}$ XSTAR grid. The warm absorber properties are parametrized in Table B2.

### 3.2.3 Absorbed Seyfert spectra – partially covering

A reasonable fraction of the AGN in this sample (16/46) require the application of a partial covering geometry whereby some fraction of the underlying power law is subject to an extra zone of absorbing gas (parameters tabulated in Table B2). The majority of the partial covering scenarios here involve high column density warm absorbing zones which have their largest effect at harder X-ray energies. For example, some AGN still exhibit a hard X-ray excess at high energies >10 keV after the use of a single REFLIONX unblurred distant reflection component and require a partial coverer with $N_H \gtrsim 10^{24} \text{ cm}^{-2}$ to fully model the HXD and BAT data; see Fig. 5. In some cases extra modelling of the hard X-ray spectrum may be due to a second blurred reflector e.g. Mrk 205; see Section 3.4. Because of the nature of a partial coverer with such a high column, not much interference with residuals in the Fe K region except at the Fe K edge is expected (see discussion in Patrick et al. 2011b, Section 3.3.1).
<figure><img src="image_4.png" /><figcaption>**Figure 3.** Ratio plots of the 4–9 keV residuals modelled with the baseline model minus *REFLIONX*, narrow lines and Fe K absorbers, i.e. the Fe K region is left totally unmodelled with only warm absorption at soft X-ray energies being taken into account in addition to the intrinsic *POWERLAW* and *COMPTT* (where required). The data have been refitted after the removal of components. The vertical dashed lines represent 6.4 keV in the observed frames. Red data points indicate those from further observations.</figcaption></figure>

In some objects, residuals remain above 10 keV even after applying a reflection component such as an unblurred *REFLIONX* can be significant, see Fig. 5, also see Turner et al. (2009) as example of the presence of a strong Compton-thick partial coverer.

Five AGN (NGC 1365, NGC 3227, NGC 3516 and NGC 4151) are best fitted with a lower column density partial coverer with $N_H \sim 10^{23} \text{ cm}^{-2}$, which adds curvature (i.e. a small, shallow bump) at >2 keV. Of course, in this region of the X-ray spectrum, there is likely to be some degree of interplay between the partial covering parameters (e.g. covering fraction, column density and ionization) and the strength of ‘broad’ residuals in the Fe K region. Note that the partial coverer properties in NGC 1365 vary between each of the three *Suzaku* observations, in particular the second observation (OBSID: 705031010) requires an additional neutral absorber,

i.e. POWERLAW+XSTAR*ZPHABS*POWERLAW. Only IRAS 13224–3809 features a partial coverer with a lower column density of $N_H \sim 10^{22} \text{ cm}^{-2}$, which models small residuals remaining in the 2–4 keV spectrum. The 2–10 keV *Suzaku* spectrum of IRAS 13224–3809 only has a small number of counts and subsequently no great deal of information can be gathered regarding any partial covering scenario. It should be noted that the majority of the partially covering zones in this sample are of low to neutral ionization.

### 3.2.4 Highly ionized absorption and outflows

A total of 14/46 (30 per cent) of the AGN in this sample feature highly ionized absorption at a minimum of the 90 per cent
<figure><img src="image_5.png" /><figcaption>Figure 3 – continued</figcaption></figure>

confidence level. A substantial proportion (10/46) of AGN in this sample are found to possess highly ionized zones which are somewhat blueshifted with respect to absorption lines from Fe xxv and Fe xxvi at rest-frame energies of 6.7 and 6.97 keV (3C 111, 3C 445, MCG-06-30-15, MR 2251-178, Mrk 766, NGC 1365, NGC 3227, NGC 3516, NGC 3783, NGC 4051, NGC 4151, NGC 5548, PDS 456 and PG 1211+143). All of these zones (bar those in NGC 3783 and NGC 5548) are outflowing, i.e. the absorption lines are blueshifted to higher energies with typical velocities of a few thousand km s⁻¹ and column densities 1 × 10²¹ ≲ N_H ≲ 1 × 10²⁴ cm⁻²; see Table B3. We note that the absorption zones in NGC 3227, NGC 3516, NGC 3783 and NGC 5548 have outflow velocities which are consistent with zero, i.e. 10/46 (22 per cent) of the AGN in this sample require highly ionized outflows at greater than the 90 per cent confidence level.

### 3.2.5 Soft excess and reflector properties

The majority of the AGN in this sample show both soft and hard X-ray excesses above the basic intrinsic power law. A substantial 31/46 AGN indicate an observed soft excess below ~2 keV (modelled as described in Section 3.1.1); however, this is lower than the fraction obtained by Porquet et al. (2004) in a selection of PG quasars who found that 19/21 objects exhibited a significant soft excess. It should be noted, however, that nearly all of the objects without a soft excess feature complex warm or neutral absorption. This can lead to any weak soft excess which may be present being ‘hidden’ or simply absorbed, thereby leaving little trace or indication of its presence. Only MCG-02-14-009 and NGC 3147 are without additional absorption (either neutral or ionized) and still show no indications of a soft excess, whereas SWIFT J2127.4+5654 has
<figure><img src="image_6.png" /><figcaption>Figure 3 – continued</figcaption></figure>

sufficiently strong neutral absorption (no warm absorption) to mask
the presence of a soft excess.

A large number of AGN in this sample also exhibit strong ex-
cesses at hard X-ray energies, indicative of reflection off distant
material, e.g. the putative torus or outer accretion disc. 39/46 of
objects in the sample are modelled using the REFLIONX reflection
model, with properties such as ionization and iron abundance Z<sub>Fe</sub>
left free to vary. The vast majority of AGN modelled using REFLIONX
here are well fitted with a neutral or close to neutral reflector (ξ <
60 erg cm s<sup>-1</sup>) with only Ton S180 featuring a moderately ionized
reflector (ξ ~ 270 erg cm s<sup>-1</sup>). The remainder of the objects without
a strong reflection component still feature neutral Fe Kα emission;
however, IRAS 13224-3809 features neither a reflection compo-
nent nor 6.4-keV Fe Kα emission.

In the majority of these AGN, the reflection component is well
modelled with solar iron abundance and in 23/39 of objects with
evidence for strong reflection it is fixed at Z<sub>Fe</sub> = 1.0. This fraction

includes the scenario in which some proportion of the observed
narrow Fe Kα flux additionally arises from material which may be
in the BLR, i.e. the Fe Kα core also originates from both reflection
off distant matter and the Compton-thin BLR. We should note that
if we assume Fe K emission from the BLR, this does not necessitate
the addition of a further reflection component such as REFLIONX.
This geometry is most evident when the strength of the narrow core
is disproportionately stronger than the strength of other reflector
features such as the Compton hump, often indicated by what may
be an unfeasibly high iron abundance, e.g. Z<sub>Fe</sub> > 3.0 being forced
into the fits. We account for this by freezing Z<sub>Fe</sub> = 1.0 and including
an additional narrow Gaussian ~6.4 keV (such as in MCG-05-23-
16, Mrk 110, Mrk 509, NGC 2992, NGC 3147, NGC 3516, NGC
4151, NGC 4593 and NGC 7213). We note, however, that if this
additional Fe Kα component originates from the BLR, it might be
expected that the σ<sub>width</sub> be higher e.g. up to σ ~ 0.10 keV. While
the exact origin of the line may be unknown, we keep σ = 0.01 keV
<figure><img src="image_7.png" /><figcaption>Figure 3 – continued</figcaption></figure>

for consistency with the other additional narrow lines used in the models, noting that some moderate broadening consistent with BLR widths cannot be ruled out.

Only 4/39 of the remaining objects still require a slightly super-solar iron abundance, namely 3C 120, Fairall 9, Mrk 335 and Ton S180. Slightly subsolar iron abundance reflectors are found in 12/46 of objects and a good fit is found to both the Compton hump in the HXD and the flux of the narrow Fe Kα core with few residuals remaining. NGC 3227 and NGC 4051 (Lobban et al. 2011) are best fitted with a subsolar iron abundance in conjunction with a narrow 6.4-keV Gaussian. This is in a similar fashion to above whereby the narrow Fe Kα flux exceeds that expected from a simple solar abundance reflector; however, both of these objects appear to still have weaker relative reflection components, i.e. a subsolar reflector plus narrow Gaussian is preferred. This may represent the scenario whereby the Fe Kα line either additionally or predominantly arises in Compton-thin material such as the BLR or NLR rather

than the outer regions of the accretion disc or torus. The baseline model parameters for each object and observation are summarized in Tables B2 and B3. Of the objects which do not require a reflection component, only IRAS 13224–3809 does not feature a narrow neutral Fe K line of any kind, while the narrow iron line in both 3C 111 and MR 2251–178 is near neutral at ~6.5 keV.

### 3.2.6 Additional distant ionized emission

We examine the Fe K regions of these AGN to determine whether emission lines due to ionized H-like and He-like species of iron are present, making up the final piece in our baseline models for each object. Lines at 6.63–6.70 and 6.97 keV are (likely due to Fe xxv and Fe xxvi, respectively) emitted from highly ionized gas existing at large distances from the central SMBH. The presence of such lines has been well documented in many Seyfert 1 spectra and it should come as no surprise that they appear relatively common in this
<figure><img src="image_8.png" /><figcaption>Figure 3 – continued</figcaption></figure>

sample (Bianchi et al. 2004; Nandra et al. 2007; Bianchi et al. 2009; Patrick et al. 2011a). Approximately half (24/46) of the objects in this sample show evidence for Fe xxv emission at ~6.7 keV, while fewer (18/46) show evidence for Fe xxvi at 6.97 keV (Table B3). However, the lower fraction of H-like Fe detections may be due to its proximity to Fe Kβ at 7.056 keV which is included self-consistently in all objects in addition to the narrow 6.4-keV Fe Kα core.

## 3.3 Broad residuals in the Fe K region

We first attempt to parametrize the strength of any broad residuals which may remain in the Fe K regions of these objects by including a broad Gaussian with line energy, $\sigma_{width}$ and normalization left free to vary. If this broad Gaussian component proves to be statistically significant at the 90 per cent level (three additional parameters, i.e. an improvement to the fit of $\Delta\chi^2 > 6.3$), we then proceed to add more physical models of the line emission form the inner regions of the accretion disc. Fig. 3 shows ratio plots of the 4–9 keV region prior to any model of reflection or disc emission components, i.e. the Fe K band is left unmodelled.

Indeed, not all of the objects in the sample require any further modelling and an excellent fit is found to the data. For example, no reasonable statistical improvement is made when adding a broad Gaussian component to the following AGN in this sample: 1H 0419–577, Ark 564, MCG–02-14-009, MCG–02-58-22, Mrk 110, Mrk 205, Mrk 279, NGC 4151, NGC 5548, NGC 7213, PDS

456, PG 1211+143, RBS 1124 and Ton S180 (see Table 3). The remaining AGN in the sample show at least some indications of a broad red wing in the Fe K region and therefore perhaps emission from the inner regions of the accretion disc (32/46 objects); however, it should be noted that this is only a simple parametrization and the true fraction of AGN may differ from this when a more physical model is used. From Table 3 we can estimate the mean parameters of the simple broad Gaussian at $\text{LineE} = 6.32 \pm 0.04$ keV, $\sigma_{width} = 0.470 \pm 0.051$ keV and equivalent width (EW) = 97 $\pm$ 19 eV. Of course, attempting to model an asymmetric line emission profile with a simple Gaussian can lead to a mismodelling of the Fe K region, e.g. broader Gaussians (such as those found here) are heavily influenced by the way in which the narrow Fe Kα core and Compton shoulder are modelled. Since the use of a broad Gaussian is essentially simply a means of adding curvature to the 5–7 keV region, in a sample of complex AGN featuring warm absorption/highly ionized outflows there is likely to be a reasonable amount of interplay between the width and strength of the broad line with the absorber properties.

We next replace the broad Gaussian with the RELLINE relativistic line emission model (Dauser et al. 2010). This produces a more physical asymmetric line profile taking into account effects such as relativistic Doppler broadening producing both red and blue wings. The shape of this line profile allows properties such as the inclination and emissivity index *q* of the accretion disc to be measured. We assume the emission line has a rest-frame energy of 6.4 keV and that the inner radius of the accretion disc extends down to $R_{ISCO}$
<table><caption>**Table 2.** Model applicability to each AGN. Comparison of components and features use to model each AGN; COMPTT is used to model the soft excess, an unblurred REFLIONX is used to model the reflection component if statistically required.</caption><thead><tr><th>Object</th><th>Soft excess</th><th>Reflection</th><th>Partial covering</th><th>Warm absorber</th><th>High ξ absorption</th><th>Residuals at Fe K</th></tr></thead><tbody><tr><td>1H 0419-577</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>X</td><td>X</td></tr><tr><td>3C 111</td><td>X</td><td>X</td><td>X</td><td>X<sup>a</sup></td><td>✓</td><td>✓</td></tr><tr><td>3C 120</td><td>✓</td><td>✓</td><td>X</td><td>X<sup>a</sup></td><td>X</td><td>✓</td></tr><tr><td>3C 382</td><td>✓</td><td>✓</td><td>X</td><td>✓</td><td>X</td><td>✓</td></tr><tr><td>3C 390.3</td><td>✓</td><td>✓</td><td>X</td><td>X</td><td>X</td><td>✓</td></tr><tr><td>3C 445</td><td>X</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td></tr><tr><td>4C 74.26</td><td>X</td><td>✓</td><td>X</td><td>✓</td><td>X</td><td>✓</td></tr><tr><td>Ark 120</td><td>✓</td><td>✓</td><td>X</td><td>X</td><td>X</td><td>✓</td></tr><tr><td>Ark 564</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>X</td><td>X</td></tr><tr><td>Fairall 9</td><td>✓</td><td>✓</td><td>X</td><td>X</td><td>X</td><td>✓</td></tr><tr><td>IC 4329A</td><td>X</td><td>✓</td><td>X</td><td>✓</td><td>X</td><td>✓</td></tr><tr><td>IRAS 13224-3809</td><td>✓</td><td>X</td><td>✓</td><td>✓</td><td>X</td><td>✓</td></tr><tr><td>MCG-02-14-009</td><td>X</td><td>✓</td><td>X</td><td>X</td><td>X</td><td>X</td></tr><tr><td>MCG-02-58-22</td><td>✓</td><td>✓</td><td>X</td><td>✓</td><td>X</td><td>X</td></tr><tr><td>MCG-05-23-16</td><td>✓</td><td>✓</td><td>X</td><td>X<sup>b</sup></td><td>X</td><td>✓</td></tr><tr><td>MCG-06-30-15</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td></tr><tr><td>MCG+8-11-11</td><td>X</td><td>✓</td><td>X</td><td>✓</td><td>X</td><td>✓</td></tr><tr><td>MR 2251-178</td><td>✓</td><td>X</td><td>X</td><td>✓</td><td>✓</td><td>✓</td></tr><tr><td>Mrk 79</td><td>X</td><td>X</td><td>X</td><td>✓</td><td>X</td><td>✓</td></tr><tr><td>Mrk 110</td><td>✓</td><td>✓</td><td>X</td><td>X</td><td>X</td><td>X</td></tr><tr><td>Mrk 205</td><td>✓</td><td>✓</td><td>✓</td><td>X</td><td>X</td><td>X</td></tr><tr><td>Mrk 279</td><td>X</td><td>✓</td><td>✓</td><td>✓</td><td>X</td><td>X</td></tr><tr><td>Mrk 335</td><td>✓</td><td>✓</td><td>X</td><td>X</td><td>X</td><td>✓</td></tr><tr><td>Mrk 359</td><td>✓</td><td>✓</td><td>X</td><td>X</td><td>X</td><td>✓</td></tr><tr><td>Mrk 509</td><td>✓</td><td>✓</td><td>X</td><td>✓</td><td>X</td><td>✓</td></tr><tr><td>Mrk 766</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>✓<sup>c</sup></td></tr><tr><td>Mrk 841</td><td>✓</td><td>✓</td><td>X</td><td>✓</td><td>X</td><td>✓</td></tr><tr><td>NGC 1365</td><td>X</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td></tr><tr><td>NGC 2992</td><td>✓</td><td>✓</td><td>X</td><td>X<sup>a</sup></td><td>X</td><td>✓</td></tr><tr><td>NGC 3147</td><td>X</td><td>✓</td><td>X</td><td>X</td><td>X</td><td>✓</td></tr><tr><td>NGC 3227</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td></tr><tr><td>NGC 3516</td><td>X</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td></tr><tr><td>NGC 3783</td><td>✓</td><td>✓</td><td>X</td><td>✓</td><td>✓</td><td>✓</td></tr><tr><td>NGC 4051</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td></tr><tr><td>NGC 4151</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>X</td></tr><tr><td>NGC 4593</td><td>X</td><td>✓</td><td>X</td><td>✓</td><td>X</td><td>✓</td></tr><tr><td>NGC 5506</td><td>X</td><td>✓</td><td>✓</td><td>✓</td><td>X</td><td>✓</td></tr><tr><td>NGC 5548</td><td>X</td><td>✓</td><td>X</td><td>✓</td><td>✓</td><td>X</td></tr><tr><td>NGC 7213</td><td>✓</td><td>✓</td><td>X</td><td>X</td><td>X</td><td>X</td></tr><tr><td>NGC 7314</td><td>✓</td><td>X</td><td>X</td><td>X<sup>a</sup></td><td>X</td><td>✓</td></tr><tr><td>NGC 7469</td><td>✓</td><td>✓</td><td>X</td><td>X</td><td>X</td><td>✓</td></tr><tr><td>PDS 456</td><td>✓</td><td>X</td><td>✓</td><td>X</td><td>✓</td><td>X</td></tr><tr><td>PG 1211+143</td><td>✓</td><td>X</td><td>X</td><td>✓</td><td>✓</td><td>X</td></tr><tr><td>RBS 1124</td><td>✓</td><td>✓</td><td>X</td><td>X</td><td>X</td><td>X</td></tr><tr><td>SWIFT J2127.4+5654</td><td>X</td><td>✓</td><td>X</td><td>X<sup>a</sup></td><td>X</td><td>✓</td></tr><tr><td>TON S180</td><td>✓</td><td>✓</td><td>✓</td><td>✓</td><td>X</td><td>X</td></tr><tr><td>Fraction</td><td>31/46</td><td>39/46</td><td>16/46</td><td>27/46</td><td>14/46</td><td>32/46</td></tr></tbody></table>

with a single uniform emissivity index throughout the disc i.e. the inner and outer *q* values are tied. The emissivity index scales as R⁻q, where *q* ~ 3 would be expected from the inner regions of the accretion disc and *q* > 5 would suggest that emission is very centrally concentrated, invoking a significant amount of light bending, e.g. see Miniutti & Fabian (2004). In some AGN, the broad line may not be sufficiently strong enough to constrain the emissivity index and in such cases we fix *q* = 3.0. The RELLINE model also

allows estimates to be placed upon the black hole spin parameter *a* (assuming R<sub>in</sub> = R<sub>ISCO</sub>), which varies between *a* = −0.998 for a maximally rotating retrograde SMBH and *a* = 0.998 for a maximally spinning prograde BH. Objects with multiple observations are modelled allowing for the normalization of the RELLINE component to vary, but all other parameters are tied e.g. in NGC 1365, NGC 3227, NGC 3516 and NGC 5506. The RELLINE component in 3C 120, Fairall 9, NGC 3783 and NGC 4051 is consistent with a

<footnote><sup>a</sup>Only an increase in the neutral Galactic column is required.</footnote>

<footnote><sup>b</sup>No XSTAR grid is required in MCG-05-23-16; however, additional neutral absorption is used to absorb only the intrinsic POWERLAW. Residuals in the Fe K region are considered to be present if there is an improvement of Δχ² > 6.3 with the addition of a broad Gaussian (see Table 3).</footnote>

<footnote><sup>c</sup>Only required in the 2006 observation of Mrk 766.</footnote>
<figure><img src="image_9.png" /><figcaption>**Figure 4.** Comparison of the differences between the soft X-ray modelling of the spectrum when using an XSTAR grid with turbulent velocities of $v_{\text{turb}} = 100 \text{ km s}^{-1}$ and $v_{\text{turb}} = 1000 \text{ km s}^{-1}$. These represent a power law with $\Gamma = 2$ absorbed by a fully covering absorption zone with column density $N_{\text{H}} = 1 \times 10^{22} \text{ cm}^{-2}$ and ionization log $\xi = 1$.</figcaption></figure>

constant flux held between observations (i.e. the line does not vary) and the normalization is tied as such; see Table 4.

After applying the RELLINE model a good fit is found in all the remaining objects, some of which are significantly improved with the introduction of a relativistic line emission model. Emission from the inner regions of the disc is not formally statistically required at the 90 per cent confidence level in 20/46 objects (see Table 4 for a summary of RELLINE fits for objects which required a broad Gaussian in Table 3; note that not all objects listed in the table formally require the RELLINE model). Of the remaining 26/46 objects which do require emission from the inner regions of the accretion disc (23/46 of the objects in this sample require the RELLINE model at $>99.5$ per cent confidence), we find a moderate average strength of EW = $96 \pm 10$ eV and a low accretion disc emissivity index of $q = 2.4 \pm 0.1$ at an inclination of $i = 33^\circ \pm 2^\circ$ (see Fig. 6). Alternatively fixing $a = 0.998$ and allowing $R_{\text{in}}$ to vary yield an average $R_{\text{in}} = 21 \pm 6 R_{\text{g}}$.

With the advent of high-quality broad-band X-ray data, tentative steps can be made towards placing estimates upon black hole spin. In particular, objects with multiple or deep observations may possess spectra with a sufficient number of counts and temporal information with which to form models allowing for consistent spin estimates and the variation in spectral shapes between observations, e.g. see Fig. 7. Here we make a total of 11 tentative constraints upon the spin parameter $a$ (upper and lower bounds in 5 AGN); see Section 4.3.3.

## 3.4 Dual reflector fits

If strong emission arises from reflection off the inner regions of the accretion disc producing a relativistically broadened Fe Kα line profile, the same degree of broadening and relativistic effects can also be applied to the entire reflection continuum. In this scenario, we form dual reflector fits (for those objects which do formally require a RELLINE component, see Table 4) consisting of a distant unblurred REFLIONX and a second inner REFLIONX convolved with the RELCONV kernel (Dauser et al. 2010). However, we still include a COMPTT component to model the soft excess continuum. For example, the analysis of a small sample of ‘bare’ Seyferts in Patrick et al.

<figure><img src="image_10.png" /><figcaption>**Figure 5.** Examples of the hard excesses which sometimes remain after modelling the full broad-band spectrum with a reflection component. In the baseline model we have accounted for these using high column density partial covering geometries. The black data points are XIS, the red are HXD data and the green are BAT data from Swift.</figcaption></figure>

(2011a) suggests that in order to produce the significant amount of blurring required to smooth the discrete soft emission lines into a continuum, both the spin parameter $a$ and emissivity of the disc are forced to high and extreme values ($a = 0.998$ and $q > 4$). Retaining the use of the COMPTT to model the soft excess ensures that the main feature driving the fit of the blurred reflector are the broad residuals in the Fe K region regardless of the interpretation of the soft excess.

Due to the additional hard X-ray flux produced by a dual reflector model, we test this as an alternative to high column partial covering scenarios, i.e. partial covering geometries are avoided during fitting unless no good fit can be found without a partially covering model. The iron abundance is tied between the inner and distant reflectors for consistency. The ionization of the two reflectors are initially allowed to vary but tied if both are approximately equal; this is found to be the case in all objects.

Simply replacing the RELLINE component in each model with the RELCONV\*REFLIONX convolution produces a good fit to the data in objects without partial covering, with estimated accretion disc parameters consistent with those obtained in the previous model (Table B4). This should come as no surprise since the Fe K region remains the main driver behind the fit. The dual reflector
<table><caption>**Table 3.** Broad Gaussian parametrization of Fe K region in addition to the baseline model. The symbol `-` indicates that no broad Gaussian can be fitted, i.e. no discernible reduction in $\chi^2$ whatsoever.</caption><thead><tr><th>Object</th><th>LineE (keV)</th><th>σ<sub>Broad</sub> (keV)</th><th>Broad line EW<sub>Broad</sub> (eV)</th><th>Flux<sup>a</sup></th><th>Δχ<sup>2</sup></th><th>Fe XXV emission</th><th>Fe XXVI emission</th></tr></thead><tbody><tr><td>1H 0419-577</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>X</td><td>X</td></tr><tr><td>3C 111</td><td>6.28<sup>+0.09</sup><sub>-0.05</sub></td><td>&lt;0.136</td><td>19<sup>+23</sup><sub>-9</sub></td><td>0.55<sup>+0.67</sup><sub>-0.27</sub></td><td>-11</td><td>✓</td><td>✓</td></tr><tr><td>3C 120</td><td>6.38<sup>+0.01</sup><sub>-0.01</sub></td><td>0.124<sup>+0.025</sup><sub>-0.022</sub></td><td>76<sup>+6</sup><sub>-9</sub><br>84<sup>+7</sup><sub>-10</sub></td><td>4.04<sup>+0.35</sup><sub>-0.49</sub></td><td>-75</td><td>✓</td><td>X</td></tr><tr><td>3C 382</td><td>6.45<sup>+0.09</sup><sub>-0.12</sub></td><td>0.198<sup>+0.210</sup><sub>-0.090</sub></td><td>42<sup>+18</sup><sub>-17</sub></td><td>2.45<sup>+1.07</sup><sub>-1.01</sub></td><td>-20</td><td>X</td><td>X</td></tr><tr><td>3C 390.3</td><td>6.49<sup>+0.09</sup><sub>-0.10</sub></td><td>0.320<sup>+0.256</sup><sub>-0.106</sub></td><td>86<sup>+31</sup><sub>-20</sub></td><td>3.29<sup>+1.17</sup><sub>-0.78</sub></td><td>-40</td><td>X</td><td>X</td></tr><tr><td>3C 445</td><td>6.04<sup>+0.12</sup><sub>-0.11</sub></td><td>&lt;0.436</td><td>23<sup>+30</sup><sub>-13</sub></td><td>1.07<sup>+0.58</sup><sub>-0.46</sub></td><td>-7</td><td>✓</td><td>X</td></tr><tr><td>4C 74.26</td><td>6.12<sup>+0.06</sup><sub>-0.07</sub></td><td>&lt;0.186</td><td>22<sup>+12</sup><sub>-9</sub></td><td>1.07<sup>+0.58</sup><sub>-0.46</sub></td><td>-20</td><td>✓</td><td>X</td></tr><tr><td>Ark 120</td><td>6.36<sup>+0.08</sup><sub>-0.09</sub></td><td>0.320<sup>+0.110</sup><sub>-0.090</sub></td><td>105<sup>+26</sup><sub>-24</sub></td><td>0.70<sup>+0.32</sup><sub>-0.32</sub></td><td>-12</td><td>X</td><td>✓</td></tr><tr><td>Ark 564</td><td>6.42<sup>+0.09</sup><sub>-0.08</sub></td><td>&lt;0.161</td><td>20<sup>+14</sup><sub>-13</sub></td><td>0.34<sup>+0.25</sup><sub>-0.22</sub></td><td>-3</td><td>✓</td><td>X</td></tr><tr><td>Fairall 9</td><td>5.91<sup>+0.24</sup><sub>-0.21</sub></td><td>0.505<sup>+0.187</sup><sub>-0.173</sub></td><td>49<sup>+20</sup><sub>-18</sub></td><td>1.45<sup>+0.58</sup><sub>-0.55</sub></td><td>-36</td><td>✓</td><td>✓</td></tr><tr><td>IC 4329A</td><td>6.34<sup>+0.15</sup><sub>-0.15</sub></td><td>0.551<sup>+0.119</sup><sub>-0.100</sub></td><td>61<sup>+15</sup><sub>-15</sub></td><td>7.94<sup>+1.96</sup><sub>-1.91</sub></td><td>-53</td><td>X</td><td>✓</td></tr><tr><td>IRAS 13224-3809</td><td>6.19<sup>+0.58</sup><sub>-0.65</sub></td><td>1.014<sup>+0.613</sup><sub>-0.346</sub></td><td>632<sup>+303</sup><sub>-260</sub></td><td>0.37<sup>+0.18</sup><sub>-0.15</sub></td><td>-9</td><td>✓</td><td>X</td></tr><tr><td>MCG-02-14-009</td><td>6.33<sup>+0.21</sup><sub>-0.24</sub></td><td>0.280<sup>+0.280</sup><sub>-0.130</sub></td><td>92<sup>+59</sup><sub>-56</sub></td><td>0.49<sup>+0.31</sup><sub>-0.30</sub></td><td>-3</td><td>X</td><td>✓</td></tr><tr><td>MCG-02-58-22</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>X</td><td>X</td></tr><tr><td>MCG-05-23-16</td><td>6.34<sup>+0.08</sup><sub>-0.10</sub></td><td>0.512<sup>+0.085</sup><sub>-0.078</sub></td><td>108<sup>+16</sup><sub>-17</sub></td><td>12.25<sup>+1.80</sup><sub>-1.87</sub></td><td>-15</td><td>✓</td><td>X</td></tr><tr><td>MCG-06-30-15</td><td>5.93<sup>+0.07</sup><sub>-0.14</sub></td><td>0.840<sup>+0.06</sup><sub>-0.06</sub></td><td>149<sup>+21</sup><sub>-9</sub></td><td>1.31<sup>+0.68</sup><sub>-0.66</sub></td><td>-302</td><td>X</td><td>✓</td></tr><tr><td>MCG+8-11-11</td><td>6.35<sup>+0.03</sup><sub>-0.04</sub></td><td>0.170<sup>+0.056</sup><sub>-0.042</sub></td><td>67<sup>+13</sup><sub>-12</sub></td><td>5.30<sup>+1.02</sup><sub>-0.97</sub></td><td>-73</td><td>X</td><td>✓</td></tr><tr><td>MR 2251-178</td><td>6.46<sup>+0.10</sup><sub>-0.17</sub></td><td>0.307<sup>+0.199</sup><sub>-0.100</sub></td><td>49<sup>+14</sup><sub>-14</sub></td><td>2.65<sup>+0.76</sup><sub>-0.75</sub></td><td>-26</td><td>X</td><td>X</td></tr><tr><td>Mrk 79</td><td>6.17<sup>+0.22</sup><sub>-0.27</sub></td><td>0.529<sup>+0.208</sup><sub>-0.159</sub></td><td>136<sup>+44</sup><sub>-45</sub></td><td>2.83<sup>+0.91</sup><sub>-0.93</sub></td><td>-51</td><td>✓</td><td>✓</td></tr><tr><td>Mrk 110</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>✓</td><td>X</td></tr><tr><td>Mrk 205</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>X</td><td>X</td></tr><tr><td>Mrk 279</td><td>6.59<sup>+0.26</sup><sub>-0.19</sub></td><td>&lt;0.333</td><td>20<sup>+25</sup><sub>-19</sub></td><td>0.15<sup>+0.19</sup><sub>-0.14</sub></td><td>-6</td><td>X</td><td>X</td></tr><tr><td>Mrk 355</td><td>6.27<sup>+0.13</sup><sub>-0.17</sub></td><td>0.500<sup>+0.130</sup><sub>-0.110</sub></td><td>134<sup>+42</sup><sub>-38</sub></td><td>2.28<sup>+0.72</sup><sub>-0.65</sub></td><td>-53</td><td>✓</td><td>✓</td></tr><tr><td>Mrk 359</td><td>6.40<sup>+0.06</sup><sub>-0.06</sub></td><td>&lt;0.177</td><td>88<sup>+39</sup><sub>-41</sub></td><td>0.52<sup>+0.23</sup><sub>-0.25</sub></td><td>-10</td><td>✓</td><td>X</td></tr><tr><td>Mrk 509</td><td>6.60<sup>+0.28</sup><sub>-0.14</sub></td><td>0.690<sup>+1.363</sup><sub>-0.151</sub></td><td>120<sup>+28</sup><sub>-27</sub></td><td>6.32<sup>+1.50</sup><sub>-1.42</sub></td><td>-57</td><td>✓</td><td>X</td></tr><tr><td>Mrk 766</td><td>6.66<sup>+0.11</sup><sub>-0.07</sub></td><td>0.144<sup>+0.109</sup><sub>-0.115</sub></td><td>73<sup>+27</sup><sub>-25</sub></td><td>0.81<sup>+0.30</sup><sub>-0.28</sub></td><td>-14</td><td>✓</td><td>X</td></tr><tr><td>Mrk 841</td><td>5.89<sup>+0.22</sup><sub>-0.24</sub></td><td>0.402<sup>+0.288</sup><sub>-0.173</sub></td><td>80<sup>+50</sup><sub>-37</sub></td><td>1.47<sup>+0.92</sup><sub>-0.68</sub></td><td>-20</td><td>✓</td><td>X</td></tr><tr><td>NGC 1365</td><td>6.48<sup>+0.02</sup><sub>-0.01</sub></td><td>&lt;0.028</td><td>&lt;13</td><td>&lt;0.29</td><td>-63</td><td>✓</td><td>✓</td></tr><tr><td>NGC 2992</td><td>6.51<sup>+0.14</sup><sub>-0.11</sub></td><td>0.323<sup>+0.153</sup><sub>-0.100</sub></td><td>73<sup>+28</sup><sub>-25</sub></td><td>1.39<sup>+0.53</sup><sub>-0.47</sub></td><td>-17</td><td>X</td><td>X</td></tr><tr><td>NGC 3147</td><td>6.45<sup>+0.04</sup><sub>-0.03</sub></td><td>&lt;0.066</td><td>110<sup>+51</sup><sub>-41</sub></td><td>0.21<sup>+0.10</sup><sub>-0.08</sub></td><td>-15</td><td>X</td><td>✓</td></tr><tr><td>NGC 3227<sup>b</sup></td><td>6.34<sup>+0.09</sup><sub>-0.09</sub></td><td>0.707<sup>+0.100</sup><sub>-0.087</sub></td><td>80<sup>+24</sup><sub>-23</sub></td><td>4.50<sup>+1.33</sup><sub>-1.28</sub></td><td>-124</td><td>X</td><td>✓</td></tr><tr><td>NGC 3516<sup>b</sup></td><td>6.32<sup>+0.12</sup><sub>-0.12</sub></td><td>0.874<sup>+0.118</sup><sub>-0.101</sub></td><td>151<sup>+22</sup><sub>-21</sub></td><td>6.95<sup>+1.01</sup><sub>-0.97</sub></td><td>-84</td><td>✓</td><td>X</td></tr><tr><td>NGC 3783<sup>b</sup></td><td>6.07<sup>+0.20</sup><sub>-0.18</sub></td><td>0.761<sup>+0.221</sup><sub>-0.104</sub></td><td>81<sup>+29</sup><sub>-29</sub></td><td>1.89<sup>+0.69</sup><sub>-0.68</sub></td><td>-68</td><td>X</td><td>✓</td></tr><tr><td>NGC 4051<sup>b</sup></td><td>6.23<sup>+0.17</sup><sub>-0.19</sub></td><td>0.742<sup>+0.151</sup><sub>-0.124</sub></td><td>97<sup>+38</sup><sub>-32</sub></td><td>6.38<sup>+2.51</sup><sub>-2.10</sub></td><td>-70</td><td>✓</td><td>X</td></tr><tr><td>NGC 4151</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>X</td><td>X</td></tr><tr><td>NGC 4593</td><td>6.65<sup>+0.18</sup><sub>-0.14</sub></td><td>0.368<sup>+0.289</sup><sub>-0.136</sub></td><td>87<sup>+40</sup><sub>-35</sub></td><td>1.26<sup>+0.58</sup><sub>-0.51</sub></td><td>-12</td><td>✓</td><td>X</td></tr><tr><td>NGC 5506<sup>b</sup></td><td>6.50<sup>+0.07</sup><sub>-0.09</sub></td><td>0.317<sup>+0.074</sup><sub>-0.060</sub></td><td>19<sup>+5</sup><sub>-4</sub></td><td>7.83<sup>+1.91</sup><sub>-1.51</sub></td><td>-32</td><td>✓</td><td>✓</td></tr><tr><td>NGC 5548</td><td>6.36<sup>+0.03</sup><sub>-0.10</sub></td><td>&lt;0.098</td><td>26<sup>+31</sup><sub>-22</sub></td><td>0.60<sup>+0.72</sup><sub>-0.52</sub></td><td>-5</td><td>X</td><td>X</td></tr><tr><td>NGC 7213</td><td>6.74<sup>+0.16</sup><sub>-0.16</sub></td><td>&lt;1.294</td><td>12<sup>+30</sup><sub>-9</sub></td><td>0.30<sup>+0.74</sup><sub>-0.22</sub></td><td>-4</td><td>✓</td><td>✓</td></tr><tr><td>NGC 7314</td><td>6.36<sup>+0.35</sup><sub>-0.19</sub></td><td>&lt;0.057</td><td>58<sup>+37</sup><sub>-34</sub></td><td>0.66<sup>+0.43</sup><sub>-0.39</sub></td><td>-7</td><td>X</td><td>✓</td></tr><tr><td>NGC 7469</td><td>6.32<sup>+0.06</sup><sub>-0.11</sub></td><td>0.150<sup>+0.07</sup><sub>-0.03</sub></td><td>62<sup>+928</sup><sub>-44</sub></td><td>1.55<sup>+0.70</sup><sub>-1.10</sub></td><td>-24</td><td>X</td><td>X</td></tr><tr><td>PDS 456</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>✓</td><td>✓</td></tr><tr><td>PG 1211+143</td><td>6.49<sup>+0.07</sup><sub>-0.06</sub></td><td>0.142<sup>+0.068</sup><sub>-0.061</sub></td><td>146<sup>+28</sup><sub>-44</sub></td><td>0.87<sup>+0.17</sup><sub>-0.26</sub></td><td>-5</td><td>✓</td><td>X</td></tr><tr><td>RBS 1124</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>X</td><td>X</td></tr><tr><td>SWIFT J2127.4+5654</td><td>6.32<sup>+0.24</sup><sub>-0.25</sub></td><td>0.390<sup>+0.450</sup><sub>-0.260</sub></td><td>71<sup>+53</sup><sub>-48</sub></td><td>3.43<sup>+2.56</sup><sub>-2.32</sub></td><td>-12</td><td>✓</td><td>✓</td></tr><tr><td>Ton S180</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>X</td><td>X</td></tr></tbody></table>

<footnote><sup>a</sup>Flux given in units of $10^{-5}$ photon cm$^{-2}$ s$^{-1}$.</footnote>

<footnote><sup>b</sup>Parameters other than normalization tied between multiple observations; all are tied in NGC 5506.</footnote>
<table><caption>**Table 4.** Summary of RELLINE fits to objects in which some statistical improvement is made. Line energy fixed at 6.4 keV.</caption><thead><tr><th>Object</th><th>EW (eV)</th><th>q</th><th>a</th><th>i (°)</th><th>Flux<sup>a</sup></th><th>R<sub>in</sub><sup>b</sup></th><th>Fe XXV</th><th>Fe XXVI</th><th>Δχ<sup>2</sup></th><th>χ<sup>2</sup><sub>v</sub></th></tr></thead><tbody><tr><td>3C 111</td><td>37<sup>+30</sup><sub>-17</sub></td><td>&lt;2.7</td><td>-</td><td>22<sup>+12</sup><sub>-5</sub></td><td>0.98<sup>+0.79</sup><sub>-0.44</sub></td><td>&lt;59</td><td>✓</td><td>✓</td><td>-10</td><td>1091.2/1094</td></tr><tr><td>3C 120</td><td>78<sup>+14</sup><sub>-16</sub><br>93<sup>+17</sup><sub>-19</sub></td><td>1.5<sup>+0.2</sup><sub>-0.3</sub></td><td>-</td><td>17<sup>+1</sup><sub>-1</sub></td><td>4.17<sup>+0.76</sup><sub>-0.85</sub></td><td>&lt;17</td><td>✓</td><td>X</td><td>-45</td><td>3586.4/3449</td></tr><tr><td>3C 382</td><td>57<sup>+20</sup><sub>-18</sub></td><td>2.7<sup>+1.2</sup><sub>-0.8</sub></td><td>-</td><td>30<sup>+2</sup><sub>-4</sub></td><td>2.65<sup>+0.93</sup><sub>-0.85</sub></td><td>15<sup>+14</sup><sub>-6</sub></td><td>X</td><td>X</td><td>-27</td><td>959.9/934</td></tr><tr><td>3C 390.3</td><td>142<sup>+24</sup><sub>-30</sub></td><td>2.3<sup>+0.6</sup><sub>-0.3</sub></td><td>-</td><td>49<sup>+3</sup><sub>-3</sub></td><td>4.96<sup>+0.84</sup><sub>-1.06</sub></td><td>&lt;15</td><td>X</td><td>X</td><td>-42</td><td>1457.2/1482</td></tr><tr><td>3C 445</td><td>71<sup>+48</sup><sub>-33</sub></td><td>&lt;1.6</td><td>-</td><td>&gt;45</td><td>1.05<sup>+0.71</sup><sub>-0.49</sub></td><td>&lt;332</td><td>X</td><td>X</td><td>-6</td><td>452.2/421</td></tr><tr><td>4C 74.26</td><td>48<sup>+25</sup><sub>-26</sub></td><td>&lt;1.7</td><td>-</td><td>72<sup>+17</sup><sub>-35</sub></td><td>1.82<sup>+0.94</sup><sub>-0.99</sub></td><td>&lt;89</td><td>X</td><td>X</td><td>-5</td><td>1339.7/1301</td></tr><tr><td>Ark 120</td><td>95<sup>+32</sup><sub>-26</sub></td><td>2.3<sup>+0.4</sup><sub>-0.4</sub></td><td>&lt;0.94</td><td>33<sup>+2</sup><sub>-17</sub></td><td>3.62<sup>+1.22</sup><sub>-0.99</sub></td><td>25<sup>+19</sup><sub>-7</sub></td><td>X</td><td>✓</td><td>-22</td><td>724.4/648</td></tr><tr><td>Fairall 9</td><td>54<sup>+26</sup><sub>-25</sub><br>69<sup>+18</sup><sub>-17</sub></td><td>2.9<sup>+0.5</sup><sub>-0.4</sub></td><td>0.60<sup>+0.19</sup><sub>-0.62</sub></td><td>31<sup>+4</sup><sub>-5</sub></td><td>1.49<sup>+0.72</sup><sub>-0.70</sub></td><td>4<sup>+2</sup><sub>-1</sub></td><td>✓</td><td>✓</td><td>-46</td><td>3558.7/3271</td></tr><tr><td>IC 4329A</td><td>69<sup>+13</sup><sub>-14</sub></td><td>2.3<sup>+0.3</sup><sub>-0.4</sub></td><td>-</td><td>51<sup>+4</sup><sub>-3</sub></td><td>8.25<sup>+1.54</sup><sub>-1.72</sub></td><td>37<sup>+8</sup><sub>-6</sub></td><td>X</td><td>✓</td><td>-46</td><td>2374.8/2198</td></tr><tr><td>MCG-02-14-009</td><td>142<sup>+47</sup><sub>-46</sub></td><td>2.0<sup>+0.4</sup><sub>-0.4</sub></td><td>&lt;0.88</td><td>24<sup>+10</sup><sub>-9</sub></td><td>6.64<sup>+2.20</sup><sub>-2.15</sub></td><td>&gt;13</td><td>X</td><td>✓</td><td>-12</td><td>611.6/538</td></tr><tr><td>MCG-05-23-16</td><td>94<sup>+11</sup><sub>-15</sub></td><td>2.5<sup>+0.4</sup><sub>-0.5</sub></td><td>&lt;0.50</td><td>24<sup>+3</sup><sub>-3</sub></td><td>10.16<sup>+1.19</sup><sub>-1.65</sub></td><td>9<sup>+5</sup><sub>-2</sub></td><td>X</td><td>X</td><td>-112</td><td>1471.2/1462</td></tr><tr><td>MCG-06-30-15</td><td>161<sup>+46</sup><sub>-44</sub></td><td>2.7<sup>+0.2</sup><sub>-0.1</sub></td><td>0.49<sup>+0.20</sup><sub>-0.12</sub></td><td>44<sup>+6</sup><sub>-2</sub></td><td>5.73<sup>+1.63</sup><sub>-1.57</sub></td><td>5<sup>+1</sup><sub>-1</sub></td><td>X</td><td>✓</td><td>-59</td><td>1967.8/1819</td></tr><tr><td>MCG+8-11-11</td><td>72<sup>+14</sup><sub>-14</sub></td><td>2.1<sup>+0.3</sup><sub>-0.4</sub></td><td>-</td><td>18<sup>+2</sup><sub>-2</sub></td><td>5.50<sup>+1.07</sup><sub>-1.07</sub></td><td>&lt;18</td><td>X</td><td>✓</td><td>-79</td><td>970.7/932</td></tr><tr><td>MR 2251-178</td><td>55<sup>+22</sup><sub>-12</sub></td><td>2.4<sup>+1.4</sup><sub>-1.0</sub></td><td>-</td><td>36<sup>+10</sup><sub>-4</sub></td><td>2.74<sup>+1.08</sup><sub>-0.61</sub></td><td>&lt;35</td><td>X</td><td>X</td><td>-30</td><td>947.3/898</td></tr><tr><td>Mrk 79</td><td>199<sup>+40</sup><sub>-37</sub></td><td>2.7<sup>+0.8</sup><sub>-0.6</sub></td><td>&lt;0.80</td><td>34<sup>+3</sup><sub>-3</sub></td><td>3.08<sup>+0.62</sup><sub>-0.57</sub></td><td>19<sup>+7</sup><sub>-9</sub></td><td>X</td><td>✓</td><td>-51</td><td>551.1/539</td></tr><tr><td>Mrk 335</td><td>146<sup>+39</sup><sub>-39</sub></td><td>2.6<sup>+0.5</sup><sub>-0.3</sub></td><td>0.70<sup>+0.12</sup><sub>-0.01</sub></td><td>38<sup>+2</sup><sub>-2</sub></td><td>2.52<sup>+0.67</sup><sub>-0.67</sub></td><td>32<sup>+12</sup><sub>-16</sub></td><td>✓</td><td>✓</td><td>-40</td><td>803.0/719</td></tr><tr><td>Mrk 359</td><td>76<sup>+62</sup><sub>-60</sub></td><td>3.0<sup>c</sup></td><td>-</td><td>26<sup>+12</sup><sub>-7</sub></td><td>0.46<sup>+0.38</sup><sub>-0.37</sub></td><td>&gt;56</td><td>✓</td><td>X</td><td>-4</td><td>606.2/559</td></tr><tr><td>Mrk 509</td><td>76<sup>+11</sup><sub>-11</sub></td><td>2.1<sup>+0.3</sup><sub>-0.3</sub></td><td>-</td><td>41<sup>+4</sup><sub>-3</sub></td><td>4.56<sup>+0.66</sup><sub>-0.65</sub></td><td>45<sup>+31</sup><sub>-24</sub></td><td>X</td><td>X</td><td>-31</td><td>1945.3/1868</td></tr><tr><td>Mrk 766<sup>d</sup></td><td>162<sup>+97</sup><sub>-62</sub></td><td>&gt;3.0</td><td>-</td><td>39<sup>+3</sup><sub>-4</sub></td><td>1.89<sup>+1.13</sup><sub>0.72</sub></td><td>&lt;28</td><td>✓</td><td>X</td><td>-17</td><td>1040.1/995</td></tr><tr><td>Mrk 841</td><td>161<sup>+43</sup><sub>-70</sub></td><td>3.0<sup>c</sup></td><td>-</td><td>&gt;32</td><td>2.85<sup>+0.77</sup><sub>-1.23</sub></td><td>&gt;8</td><td>✓</td><td>X</td><td>-20</td><td>917.9/854</td></tr><tr><td>NGC 1365</td><td>94<sup>+36</sup><sub>-36</sub><br>&lt;50<br>&lt;1</td><td>3.0<sup>c</sup></td><td>-</td><td>52<sup>+11</sup><sub>-2</sub></td><td>1.59<sup>+0.61</sup><sub>-0.61</sub></td><td>5<sup>+18</sup><sub>-3</sub></td><td>✓</td><td>✓</td><td>-100</td><td>2162.8/1975</td></tr><tr><td>NGC 2992</td><td>71<sup>+28</sup><sub>-31</sub></td><td>2.1<sup>+0.8</sup><sub>-0.7</sub></td><td>-</td><td>&gt;26</td><td>1.33<sup>+0.52</sup><sub>-0.58</sub></td><td>&lt;169</td><td>X</td><td>X</td><td>-12</td><td>1076.6/1075</td></tr><tr><td>NGC 3147</td><td>&lt;17</td><td>3.0<sup>c</sup></td><td>-</td><td>-</td><td>&lt;0.11</td><td>-</td><td>X</td><td>✓</td><td>-2</td><td>278.6/263</td></tr><tr><td>NGC 3227</td><td>47<sup>+23</sup><sub>-22</sub><br>125<sup>+31</sup><sub>-31</sub><br>&lt;50<br>26<sup>+4</sup><sub>-4</sub><br>48<sup>+23</sup><sub>-23</sub><br>&lt;54</td><td>2.7<sup>+0.5</sup><sub>-0.4</sub></td><td>-</td><td>33<sup>+2</sup><sub>-2</sub></td><td>2.05<sup>+0.98</sup><sub>-0.98</sub><br>2.93<sup>+0.73</sup><sub>-0.72</sub><br>&lt;1.74<br>3.85<sup>+0.62</sup><sub>-0.61</sub><br>1.49<sup>+0.71</sup><sub>-0.70</sub><br>&lt;1.32</td><td>11<sup>+3</sup><sub>-6</sub></td><td>X</td><td>✓</td><td>-120</td><td>4465.6/4189</td></tr><tr><td>NGC 3516</td><td>58<sup>+9</sup><sub>-9</sub><br>14<sup>+2</sup><sub>-2</sub></td><td>3.1<sup>+0.4</sup><sub>-0.2</sub></td><td>&lt;0.30</td><td>&lt;41</td><td>2.79<sup>+0.42</sup><sub>-0.43</sub><br>0.39<sup>+0.14</sup><sub>-0.13</sub></td><td>8<sup>+1</sup><sub>-1</sub></td><td>✓</td><td>X</td><td>-55</td><td>1208.3/1121</td></tr><tr><td>NGC 3783</td><td>57<sup>+12</sup><sub>-16</sub><br>46<sup>+10</sup><sub>-13</sub></td><td>3.2<sup>c,e</sup></td><td>&lt;0.24</td><td>&lt;23</td><td>3.72<sup>+0.80</sup><sub>-1.06</sub></td><td>8<sup>+1</sup><sub>-2</sub></td><td>X</td><td>✓</td><td>-64</td><td>2490.5/2302</td></tr><tr><td>NGC 4051</td><td>81<sup>+32</sup><sub>-25</sub><br>40<sup>+15</sup><sub>-12</sub><br>41<sup>+16</sup><sub>-13</sub></td><td>3.0<sup>c</sup></td><td>-</td><td>&lt;20</td><td>1.09<sup>+0.42</sup><sub>-0.34</sub></td><td>9<sup>+1</sup><sub>-1</sub></td><td>✓</td><td>X</td><td>-18</td><td>3187.2/2939</td></tr><tr><td>NGC 5506</td><td>30<sup>+10</sup><sub>-11</sub><br>53<sup>+12</sup><sub>-12</sub></td><td>1.9<sup>+0.4</sup><sub>-0.5</sub></td><td>-</td><td>20<sup>+5</sup><sub>-3</sub></td><td>4.82<sup>+1.67</sup><sub>-1.73</sub><br>7.92<sup>+1.85</sup><sub>-1.78</sub></td><td>&lt;21</td><td>✓</td><td>✓</td><td>-50</td><td>3139.3/2867</td></tr><tr><td>NGC 7314</td><td>56<sup>+44</sup><sub>-41</sub></td><td>&lt;4.6</td><td>-</td><td>&lt;89</td><td>0.58<sup>+0.46</sup><sub>-0.43</sub></td><td>&lt;164</td><td>X</td><td>✓</td><td>-4</td><td>588.3/541</td></tr><tr><td>NGC 7469</td><td>91<sup>+9</sup><sub>-8</sub></td><td>1.7<sup>+0.4</sup><sub>-0.6</sub></td><td>0.69<sup>+0.09</sup><sub>-0.09</sub></td><td>23<sup>+15</sup><sub>-7</sub></td><td>2.23<sup>+0.22</sup><sub>-0.20</sub></td><td>81<sup>+82</sup><sub>-37</sub></td><td>X</td><td>X</td><td>-25</td><td>815.5/808</td></tr><tr><td>SWIFT J2127.4+5654</td><td>178<sup>+82</sup><sub>-69</sub></td><td>2.6<sup>+1.0</sup><sub>-0.4</sub></td><td>0.70<sup>+0.10</sup><sub>-0.14</sub></td><td>43<sup>+5</sup><sub>-10</sub></td><td>6.35<sup>+2.91</sup><sub>-2.46</sub></td><td>&lt;33</td><td>X</td><td>X</td><td>-37</td><td>852.3/867</td></tr></tbody></table>

<sup>a</sup>Flux given in units of 10<sup>-5</sup> photon cm<sup>-2</sup> s<sup>-1</sup>.

<sup>b</sup>Inner radius of emission is quoted as an alternative to the spin parameter *a*, i.e. spin is frozen at maximal (*a* = 0.998) and the inner radius is allowed to vary away from *R*<sub>ISCO</sub>.

<sup>c</sup>A frozen parameter.

<sup>d</sup>RELLINE component is only employed in the 2006 observation of Mrk 766.

<sup>e</sup>Emissivity frozen at best-fitting value from Patrick et al. (2011b).
<figure><img src="image_11.png" /><figcaption>**Figure 6.** νFν plots of the baseline+RELLINE model in the 4–9 keV region. Note the strong absorption in the Fe K region in many objects and relatively weak red wing. The solid black line shows the total model.</figcaption></figure>

approach as an alternative to partial covering provides a reasonable fit to Mrk 766 ($\Delta\chi^2 = 1109.6/1002$); however, this is notably worse than when the use of a partial covering geometry is retained ($\chi^2_ν = 1055.1/995$). A poor fit is obtained to all three observations of NGC 4051 without invoking partial covering ($\chi^2_ν = 3321.9/2943$ versus $\chi^2_ν = 3177.1/2939$) while keeping the iron abundance of both reflectors tied ($Z_{Fe} = 1.0$); however, disc parameters are forced to extreme values (i.e. $q > 7$ and $a = 0.998$). In addition to this, the 2–100 keV blurred reflector flux of the 2005 observation is approximately 2–3 times that of the 2008 observations despite being in a far more absorbed state (see Fig. 7), we therefore retain the use of a partial coverer due to both physical and statistical arguments (see relevant section in the appendix for more details on NGC 4051).

A poor and statistically inferior fit to the broad-band data is found in some objects when a high column partial coverer is replaced with a dual reflector as an alternate mechanism for accounting for ad-

ditional hard X-ray flux above 10 keV. For those objects which feature a broad iron line, a partial covering geometry is still statisti- cally required in Mrk 766, NGC 1365, NGC 3227, NGC 3516 and NGC 4051 (Table B4). Treating these AGN as above and replacing RELLINE with RELCONV\*REFLIONX while still including a partial cov- erer again produce a good fit to the data with consistent accretion disc parameters to those in Table 4 (see Table B4). Removing the partial coverer and accounting for the hard excess with the inner reflector yields an improved fit to MCG−06-30-15 and NGC 5506 (i.e. 2/16); however, the parameters obtained are consistent with those estimated with a partial covering geometry.

## 4 DISCUSSION

This sample of 46 objects includes all the Seyfert 1 AGN match- ing our selection criteria outlined in Section 2.1 with observations
<figure><img src="image_12.png" /><figcaption>Figure 6 – continued</figcaption></figure>

which are publicly available in the *Suzaku* archive. The aim of this
paper is to form detailed broad-band models for each object, fully
modelling and accounting for any absorption where required which
then allows us to parametrize the Fe K regions and ultimately see
in how many objects we can estimate or constrain SMBH spin.
The main motivation for conducting this analysis is to produce an
in-depth study of the Fe K regions of these AGN and to assess the
strength and prevalence of broad emission from the inner regions
of the accretion disc. In order to accurately examine both emission
and absorption properties in the Fe K region, it is essential that
high-energy data are used to measure the strength of the Compton
hump and hard X-ray excess as part of the formation of a broad-
band model; the *Suzaku* X-ray observatory is unique in its ability
to provide such data simultaneously with soft X-ray data. The data
included in this sample have been selected with sufficient S/N such
that, if broadened line emission from the inner regions of the accre-
tion disc exists (down to tens of eV in EW), we should be able to
detect it.

It should be noted that the broad-band X-ray spectra of these
AGN are complex with many of them featuring multiple absorption
zones which have a significant role in adding spectral curvature and
hence have a significant effect upon and ‘broad’ residuals in the Fe K
region. Nandra et al. (2007) also note that the continua are complex
in a study of the 2.5–10.0 keV energy band with data obtained with
*XMM-Newton*; however, here we take this study a step further by
also considering a detailed modelling of the 0.6–10.0 keV soft X-ray
data, allowing us to form more complete models of the entire X-
ray spectrum up to 100 keV. Low-energy X-ray data below 2.5 keV
are essential to perform a detailed analysis of the Fe K region of
any object since first forming an appropriate baseline model, with
soft X-ray warm absorption included, is an important prerequisite.
This is due to the warm absorption zones which are required to
<figure><img src="image_13.png" /><figcaption>Figure 6 – continued</figcaption></figure>

model the X-ray data below 2.5 keV can add significant spectral
curvature above 2.5 keV and therefore influence the Fe K region
and residuals which may otherwise be interpreted as a broad red
wing from the very inner regions of the accretion disc, for example
see MCG-06-30-15 (Patrick et al. 2011b).

**4.1 Ionized emission in the Fe K region**

Narrow ionized emission from distant material is found to be rela-
tively common (in the baseline model) amongst these Seyfert 1 AGN
with 24/46 (52 per cent) of objects featuring Fe XXV emission at
6.63–6.7 keV and 18/46 (39 per cent) featuring Fe XXVI emission
at ~6.97 keV. Meanwhile 10/46 objects feature both Fe XXV and
Fe XXVI emission (Table B3). These fractions are much higher than
those obtained by Nandra et al. (2007) who only find significant
emission at 6.7 keV in NGC 5506 and significant 6.97-keV emis-
sion in both NGC 3783 and NGC 4593. Comparing to Fukazawa

et al. (2011), we also find a higher fraction here; however, this may
be due to our more stringent selection criteria (e.g. >30 000 counts
and exposure >50 ks) and hence an increased ability to detect a
weaker ionized line in the data if it is indeed present. The findings
here, however, concur with those found by Bianchi et al. (2009) and
Patrick et al. (2011a) who similarly find that narrow ionized emis-
sion lines are a common feature of a number of Seyfert 1 spectra.

After the inclusion of a component such as RELLINE to account
for any broad iron line residuals, however, these fractions can be
somewhat reduced due to interplay with the blue wing of a relativis-
tically broadened line profile falling in the 6.6–7.0 keV region in
some AGN. For example, a feature at ~6.7 keV can often be mod-
elled as either narrow ionized emission or as part of a broad-line
profile with fairly typical emissivity and inclination parameters. It
is likely, therefore, that the true fraction of Seyfert 1 spectra with
narrow ionized emission (Fe XXV in particular) is lower after the
inclusion of a broad-line component. In four objects the feature
<figure><img src="image_14.png" /><figcaption>Figure 6 – continued</figcaption></figure>

at ~6.7 keV is preferentially described by a relativistic line profile for the above reasons, leaving the final number of AGN in this sample with distant Fe XXV emission as 18/46 objects. Calorimeter resolution spectra from Astro-H will help to resolve these issues.

## 4.2 Absorption in the Fe K region

In addition to absorption at soft X-ray energies, absorption in the Fe K region due to 1s–2p resonance lines from Fe XXV and Fe XXVI is found to be relatively common amongst the AGN in this sample. Evidence for highly ionized absorption is found in 14/46 (30 per cent): 3C 111, 3C 445, MCG–6-30-15, MR 2251–178, Mrk 766, NGC 1365, NGC 3227, NGC 3516, NGC 3783, NGC 4051, NGC 4151, NGC 5548, PDS 456 and PG 1211+143; consistent with the 36 per cent detected by Tombesi et al. (2010b) in a larger sample of 101 XMM-Newton observations searching for ultra-fast outflows (UFOs). The majority (10/14) of these lines are blueshifted, suggesting that they originate from an outflowing zone of absorbing gas. When modelled with a high turbulent velocity $v_{\text{STAR}}$ grid ($v_{\text{turb}} = 1000 \text{ km s}^{-1}$), we find a mean column density $N_{\text{H}} = (1.74 \pm 0.85) \times 10^{23} \text{ cm}^{-2}$, mean ionization log($\xi$) = 3.97 ± 0.13 and a wide range in outflow velocity ranging $400 < v_{\text{out}} < 84\,600 \text{ km s}^{-1}$ with no clear peak in the distribution of $v_{\text{out}}$ values (as shown in Fig. 8). More details regarding highly ionized and outflowing zones will appear in a forthcoming paper (Gofford et al., in preparation), which performs a more exhaustive statistical search for blueshifted Fe K absorption lines.

We must note that these highly ionized zones can influence the strength of any broad residuals in the Fe K region, e.g. Reeves et al. (2004) found that no broad residuals remained in an XMM-Newton observation of NGC 3783 after the application of the required XSTAR grid to model the highly ionized absorption. The measured strength of any ‘broad’ residual is therefore reduced, given an appropriate high $\xi$ absorption zone and hence the detection and modelling of such zones are essential if robust statistics regarding the Fe K region are to be formed. Based upon the work by Tombesi et al. (2010a,b), the actual fraction of AGN with statistically significant outflows may indeed be higher than the 30 per cent found here

due to the presence of UFOs with absorption lines blueshifted to >7 keV since we have not systematically searched for these from 7 to 10 keV (see Gofford et al., in preparation). The fraction of AGN with highly ionized zones presented here may also in fact be larger. It is possible that the presence of narrow emission lines from ionized species of iron may reduce our ability to detect absorption lines in CCD resolution spectra from the same species of iron with current instruments.

## 4.3 Broad emission in the Fe K region

After the formation of a complete baseline model, we introduce the physically motivated relativistic line emission model RELLINE to account for any remaining broad residuals in the Fe K region. The criterion for the presence of a broad component is $\Delta\chi^2 > 7.8$ with the introduction of four additional free parameters ($q, a, i$ and normalization); this is equivalent to the 90 per cent confidence level. Based upon this requirement, we find that 26/46 (i.e. 57 per cent, Table 5) of the AGN (by object, not observation) in this sample formally statistically require relativistic emission from the inner regions of the accretions disc. Furthermore, 23/46 (50 per cent, Table 4) require broadened line emission at >99.5 per cent confidence ($\Delta\chi^2 > 15$). This fraction is somewhat lower (although not substantially so) than that obtained by Nandra et al. (2007) who find that 18/26 (69 per cent) of objects in their sample show evidence for broad-line emission at >99 per cent confidence. The slight disparity between the two surveys may be due to the energy range over which the analysis has been conducted: 0.6–100.0 keV here, versus 2.5–10.0 keV. This study also takes into account partial covering where required. However, the slight difference may be due to the smaller number statistics in the Nandra et al. (2007) sample. In a flux-limited sample, de la Calle Pérez et al. (2010) find 11/31 of objects (36 per cent) feature relativistic iron lines.

### 4.3.1 Average parameters of the disc

Taking the parameters obtained with RELLINE for the 26 objects featuring broadened line emission (Table 4), we can estimate the
<figure><img src="image_15.png" /><figcaption>**Figure 7.** νFν plots of the full broad-band models of some objects displaying significant variability. Note that the 2005 (black) observation of NGC 3516 is of higher flux, yet appears to be more absorbed, whereas in the majority of these examples it intuitively appears that simply the covering fraction has varied between observations.</figcaption></figure>

typical parameters of the accretion disc (Table 6). The average inclination of the disc is $i = 33^\circ \pm 2^\circ$ for 21 objects, consistent with Nandra et al. (2007) who find $i = 38^\circ \pm 6^\circ$. The average emissivity index of the disc is measured at a low to moderate $q = 2.4 \pm 0.1$ (for the 20 objects in which it can be constrained) and is consistent with an analysis of six ‘bare’ Seyferts by Patrick et al. (2011a) and an XMM–Newton survey by de la Calle Pérez et al. (2010) who find $q = 2.4 \pm 0.4$ and $i = 28^\circ \pm 5^\circ$. This value is much lower compared to an often high emissivity ($q > 5$) assumed by many light-bending models (Miniutti & Fabian 2004; Miniutti et al. 2009; Brenneman et al. 2011; Gallo et al. 2011; Nardini et al. 2011), suggesting that strong GR effects may not be present in the X-ray spectra of these Seyfert AGN. Fig. 9 shows the distribution of the emissivity indices for the sample; note that there is a relatively small dispersion in $q$ with the majority of values centred around $q \sim 2.4$.

The average strength of the RELLINE component is measured at EW = 96 ± 10 eV for the total of 26 objects, consistent within errors with Patrick et al. (2011a) and Nandra et al. (2007). The typical EWs of the line component are also largely consistent with Fukazawa et al. (2011) who parametrize all of the 6.4 keV narrow

and broad emission with a single Gaussian in a large Suzaku sample of Seyfert 1 and 2 AGN. As can be seen from Fig. 9, there is a wide range in the measured EWs of the RELLINE component, revealing a possible bimodal nature with a group centring around EW ~ 70 eV and a second stronger though less populated group at EW ~ 150 eV. Although there are insufficient statistics in this sample to draw any conclusions from this, indeed the distribution may be more continuous when taking error bars and different confidence levels into account. It is also interesting to note that in the cases where BH spin can be constrained, maximal spin is ruled out in all objects with the spin parameter *a* preferring to take low to intermediate values, similarly the typical inner radius of emission is at tens of $R_g$ with many clustered around $R_{in} \sim 20–30 R_g$ (see Fig. 9).

When parametrized with a Gaussian, we find an average line centroid energy of LineE = 6.32 ± 0.04 keV (see Fig. 10), $\sigma_{width} = 0.47 \pm 0.05$ and EW = 97 ± 19 eV (Table 6), both of which are also consistent with a similar parametrization with a broad Gaussian by Nandra et al. (2007) who find an average LineE = 6.27 ± 0.07 keV, EW = 91 ± 13 eV, respectively. In an analysis of the 2–10 keV spectrum of 149 radio-quiet Type 1 Seyfert AGN with
<figure><img src="image_16.png" /><figcaption>**Figure 8.** The distribution of ionization and outflow velocity of absorption zones at Fe K energies. Note that the outflow velocity covers a wide range of velocities with no clear peak within the parameter space.</figcaption></figure>

<table><caption>**Table 5.** Table of main model components and the percentage of objects in the sample of 46 objects which feature those components based upon >90 per cent confidence levels.</caption><thead><tr><th>Component</th><th>Percentage</th></tr></thead><tbody><tr><td>Soft excess</td><td>67 ± 6 per cent</td></tr><tr><td>Reflection</td><td>85 ± 6 per cent</td></tr><tr><td>Warm absorber</td><td>59 ± 5 per cent</td></tr><tr><td>Partial covering</td><td>35 ± 4 per cent</td></tr><tr><td>Fe K outflow</td><td>30 ± 4 per cent</td></tr><tr><td>Fe XXV emission</td><td>52 ± 5 per cent</td></tr><tr><td>Fe XXVI emission</td><td>39 ± 4 per cent</td></tr><tr><td>Broad Fe Kα line</td><td>57 ± 5 per cent</td></tr></tbody></table>

XMM–Newton, de la Calle Pérez et al. (2010) estimate a mean broad-line EW = 143 ± 27 eV, which is higher than that obtained here; however, the authors note that this may be an overestimate due to an inability to detect weak lines and a bias towards higher values.

Note that when obtaining measurements for the emissivity index of the disc and subsequently the spin of the SMBH, the way in which the soft excess is modelled can have a significant effect. For example, if the soft excess is not modelled according to a soft Comptonization origin (e.g. COMPTT or to a lesser extent DISKBB) and instead an atomic origin is preferred, the disc parameters are drastically altered; see Section 3.1.1.

<table><caption>**Table 6.** Average parameters of the sample; values quoted for a broad Gaussian and RELLINE are for those objects in which those components were statistically significant at >90 per cent confidence level.</caption><thead><tr><th>Parameter</th><th>Average value</th></tr></thead><tbody><tr><td colspan="2">POWERLAW</td></tr><tr><td>Γ</td><td>1.82 ± 0.03</td></tr><tr><td colspan="2">Broad Gaussian</td></tr><tr><td>Energy (keV)</td><td>6.32 ± 0.04</td></tr><tr><td>EW (eV)</td><td>97 ± 19</td></tr><tr><td>σ<sub>width</sub> (keV)</td><td>0.47 ± 0.05</td></tr><tr><td colspan="2">RELLINE</td></tr><tr><td>EW (eV)</td><td>96 ± 10</td></tr><tr><td>q</td><td>2.4 ± 0.1</td></tr><tr><td>R<sub>in</sub> (R<sub>g</sub>)</td><td>21 ± 6</td></tr><tr><td>Inclination (°)</td><td>33 ± 2</td></tr></tbody></table>

### 4.3.2 Shape of the line profile

The emissivity index obtained here is based primarily upon any remaining residuals in the Fe K region, i.e. RELLINE is modelling a relativistic line profile which takes into account both red and blue wings of a line profile rather than simply adding a broad ‘hump’ to the data below 6.4 keV (as, for example, a Gaussian might). It should be noted that for moderate to high inclinations ($i \gtrsim 20^{\circ}$) the blue wing of the line profile peaks at a higher flux than the red-wing peak, due to a boosting effect from material travelling at relativistic velocities in orbit ‘close’ to the central black hole. This effect is accentuated with lower emissivities, since with increasing $q$ (and hence more centrally concentrated emission) a greater proportion of the emitted photons are present in the red wing of the line profile due to their proximity to the very inner regions and increased gravitational broadening. At particularly high emissivities, the blue wing diminishes and the majority of the flux is contained within the red wing of the line profile, forming a single peaked profile and an increasingly strong red wing below 6.4 keV (Fabian et al. 1989; Laor 1991; Dauser et al. 2010). Further still, at near-maximal spin and high $q$ the entire line profile can produce an asymmetric featureless hump which simply creates additional curvature in the ~1–7 keV region.

Despite the narrow nature of the blue wing at low $a$ and $q$, its strength relative to the red wing (and continuum) is typically insufficient to provide an alternative explanation for narrow emission lines commonly attributed to distant Fe XXV (at ~30°) or Fe XXVI emission (at ~40°). However, there should be some caution to account for the presence of narrow ionized emission lines prior to applying a relativistic line model to ensure that the correct inclination of the disc is measured.

The driving factor behind the estimated emissivity and spin values is therefore primarily the strength and width of the red wing. Fig. 10 indicates that when modelled with a broad Gaussian, the typical line centroid energy of the broad line peaks at 6.3–6.4 keV, which also suggests that any broad emission in the Fe K region is not strongly gravitationally redshifted. The low average emissivity index ($q = 2.4 \pm 0.1$) of the disc found in this sample of 46 objects is as a result of a full and thorough modelling of the broad-band spectrum, i.e. after including XSTAR grids for the required absorption zones which dominate the spectrum in many objects below 2.5 keV, we note that the associated spectral curvature these zones add at higher energies (Miller et al. 2008; Zycki et al. 2010) leave little room
<figure><img src="image_17.png" /><figcaption>**Figure 9.** Figures of the distribution of emissivity index, RELLINE equivalent width, SMBH spin and inner radius of emission. Note that the typical inner radius of the disc for the sample centres around tens of $R_g$.</figcaption></figure>

for a significantly broadened relativistic line profile with high *q* and maximal spin. The extremely centrally concentrated emission that emissivities of *q* ≳ 4 suggest are simply no longer required and relativistic emission from the disc (if present) originates from regions more distant to the BH (typically tens of $R_g$, see Table 4 and Fig. 9).

The strength of the iron line profile has been noted to vary in a number of objects over long time-scales and also over the course of a single observation (e.g. Matsumoto et al. 2003; Miyakawa et al. 2009; Risaliti et al. 2009). It is indeed possible that the analysis of the time-averaged spectrum may instead produce an artificial broad-line profile which is simply an average line profile which could therefore result in inaccurately derived disc properties. It is likely, however, that the changes in the observed line profile are in fact a consequence of changes in the warm absorber or partial covering properties. For example, over the six *Suzaku* observations of NGC 3227 the EW of the broad iron line is seen to vary greatly when the absorber properties are fixed between each observation (i.e. by hundreds of eV); however, allowing the ionization of the partial coverer to vary significantly reduces the requirement for a strong broad line, instead resulting in typical EW ~ 50 eV. Allowing for such absorber changes on medium to long-term time-scales to account for spectral variability can therefore drastically alter the measured Fe K line profile (Miyakawa et al. 2009; Risaliti et al. 2009).

### 4.3.3 SMBH spin

With the use of broad-band data from observatories such as *Suzaku*, we can make tentative steps towards estimating the spin of the central SMBH. The primary effect of the spin parameter *a* upon the line profile is to set the degree to which the red wing extends to

the soft X-ray energies, i.e. a maximal Kerr black hole would have the smallest inner radius of the accretion disc, thereby subjecting emitted photons to a stronger redshift and sharply extending the red wing well into the soft X-ray regime. A Schwarzschild black hole ($a=0$), however, truncates the red wing of the line profile at ~4 keV due to a minimum inner radius of 6 $R_g$ and less pronounced redshift-ing of emitted photons (indeed a maximally retrograde BH pushes the inner radius further out to $R_{in} \sim 9 R_g$). It is clear to see, there-fore, that if the spectral curvature associated with various warm absorbing zones is not taken into account, a relativistic line emis-sion model such as RELLINE or KERRDISK may be forced to higher near-maximal spin values to 'take up the slack' of an improperly modelled continuum.

Many of the prime candidates for measuring SMBH spin with *Suzaku* have already been presented in previous papers, first the ‘bare’ Seyferts (Patrick et al. 2011a) and a collection of deep *Suzaku* observations (Patrick et al. 2011b), hence few new BH spin estimates are presented here. In Fairall 9, NGC 3516 and NGC 3783, however, we conduct for the first time an analysis of each of the multiple *Suzaku* observations of each object, finding a baseline+RELLINE model which can accurately describe the ob-jects in different flux states with only subtle variations to the model over time, e.g. changes in continuum flux. As stated in Section 3.3, all parameters of the RELLINE component are tied between observa-tions except the normalization, i.e. the flux of the line is allowed to vary appropriately with the flux of the other primary components of the baseline model. Finding a model which can adapt over time to fit each observation while retaining the same basic properties (e.g. emissivity, inclination, spin) arguably increases the robust-ness of the results. Encouragingly, the fits to Fairall 9 and NGC 3783 are consistent with the analysis of the individual observa-tions by Schmoll et al. (2009), Emmanoulopoulos et al. (2011) and Patrick et al. (2011a,b), finding $a = 0.60_{-0.62}^{+0.19}$ in Fairall 9, ruling out
<figure><img src="image_18.png" /><figcaption>**Figure 10.** Histograms showing the distribution of line centroid energy and $\sigma_{width}$ when broadened emission in the Fe K region is modelled with a Gaussian.</figcaption></figure>

maximal spin at >95 per cent confidence with an emissivity index of $q = 2.9_{-0.4}^{+0.5}$.

In addition to the spin estimates from Patrick et al. (2011a,b), the results of this paper suggest further low to moderate SMBH spin values on MCG-05-23-16 ($a < 0.50$), Mrk 79 ($a < 0.80$) and NGC 3516 ($a < 0.30$). Out of the total of 46 objects, we find that spin constraints can be placed on 11/46 AGN, while five of these allow us to place upper and lower bounds upon $a$ and hence constrain the spin to some degree. Albeit with this small number of SMBH spin estimates, we can take tentative steps towards starting to develop a basic picture of the spin distribution of these Seyfert 1 AGN (see Fig. 9). A maximal prograde SMBH is ruled out in all of these objects at a minimum of 90 per cent confidence and >99.5 per cent confidence in 5/11 (MCG-6-30-15, NGC 3516, NGC 3783, NGC 7469 and SWIFT J2127.4+5654; see Fig. 9). The dual reflector fits in Table B4 also appear to suggest that four AGN in this sample may have retrograde SMBHs (i.e. $a < 0$; Mrk 79, NGC 3227, NGC 3516 and NGC 3783); however, a more likely scenario is the possibility of a prograde rotating BH (or even Schwarzschild) with an accretion disc truncated short of the innermost stable circular orbit (ISCO).

### 4.3.4 NGC 3783 – high or low spin?

In an analysis of the long 210-ks 2009 *Suzaku* observation of NGC 3783, Patrick et al. (2011b, hereafter P2011b) concluded that the data appeared to rule out a maximal black hole in NGC 3783 (con-

straining spin to $a < 0.31$ in a dual reflector model), while the fit could be achieved with approximate solar abundances for the reflector. However, Brenneman et al. (2011, hereafter Br2011) came to the opposite conclusion, appearing to require near-maximal black hole spin from fits to the iron line data in NGC 3783 (with $a > 0.98$ at >90 per cent confidence) and obtaining a high iron abundance of $Z_{Fe} = 3.7_{-0.9}^{+0.9}$ and a steep inner emissivity law for the innermost disc. Subsequently Reynolds et al. (2012b, hereafter Rey2012) also appeared to confirm the high-spin, high-abundance scenario in a reanalysis of the 2009 data set, suggesting that the iron abundance of the reflector and the black hole spin may be degenerate upon each other and that a statistically preferred fit can be obtained with higher abundances and higher spin.

In this section we attempt to discuss the differences between these works, by considering the long 2009 *Suzaku* observation of NGC 3783. First the model of Br2011 was reconstructed, in order to understand the difference in the spectral modelling. The main difference between the Br2011 and P2011b models is the construction of the warm absorber; in Br2011 all three zones of the warm absorber only partially cover the AGN, where a fraction of ~17 per cent of the direct continuum is unabsorbed by the warm absorber, or alternatively is scattered back into the line of sight. On the contrary in P2011b and in this paper, the warm absorber fully covers the X-ray continuum emission. Indeed we note that previous analyses have not needed to invoke partial covering in order to model the warm absorber in NGC 3783 (Reeves et al. 2004; Yaqoob et al. 2005), including high-resolution X-ray spectroscopy from XMM-Newton RGS (Blustin et al. 2002) and during a 900-ks Chandra HETG observation (Kaspi et al. 2002).

The other main difference in the model construction is that the PEXMON neutral reflection model (Nandra et al. 2007) is used for the distant (narrow) reflector in Br2011. In P2011b and in this paper, the REFLIONX ionized reflection model (Ross & Fabian 2005) is adopted, allowing the ionization state to reach a low value of $\xi = 1$ erg cm s$^{-1}$ appropriate for low-ionization iron. For the disc (i.e. blurred) reflection, both analyses use the REFLIONX table, convolved with a relativistic blurring function such as KERRCONV (Brenneman & Reynolds 2006) or RELCONV (Dauser et al. 2010). For simplicity in this section, we use the KERRCONV model, with spin allowed to vary between $a = 0$ and 0.998 for a prograde black hole. The emissivity index is modelled as a broken power-law function (where $q_1$ is the inner emissivity and $q_2$ the outer emissivity and usually $q_1 > q_2$), breaking at a disc radius of $r_b$ in units of $R_g$. The inner disc radius is set equal to the ISCO, while the outer radius is set to $400R_g$. We adopt here the solar abundances of Anders & Grevesse (1989) for the Galactic column, noting that there is little difference to the blurred reflector model parameters if the Wilms et al. (2000) interstellar medium abundances are used instead.

In order to test the Br2011 model, we use the identical energy ranges for the XIS F1 spectrum and HXD/PIN adopted by Br2011, from 0.7 to 45 keV, ignoring the 1.5–2.5 keV band in the XIS. We also used the same warm absorber model and tables as per the Br2011 and Rey2012 papers. The Br2011 model has a steep index for the inner emissivity law, a high black hole spin consistent with maximal and a high iron abundance of the inner reflector of $Z_{Fe,inner} \sim 3$, while the iron abundance of the distant reflector is initially fixed equal to solar, i.e. $Z_{Fe,outer} = 1$. This model as detailed in Br2011 initially gives a poor fit ($\chi^2 = 1501/1234$); however, subsequently refitting the model parameters then gives an excellent fit to the data, with $\chi^2 = 1329/1234$. None the less the model parameters are in good agreement with those obtained in Br2011,
where we obtain a formal 90 per cent lower limit of $a > 0.82$ to the black hole spin (for one interesting parameter), a disc inclination of $i = 22^\circ \pm 4^\circ$, while the emissivity indices have values of $q_1 = 4.4 \pm 1.2$ and $q_2 = 2.8 \pm 0.2$, with a break radius of $\sim 6 R_g$.

However, upon taking the same model and fixing the spin to $a = 0$, then the fit statistic obtained is only slightly worse, where $\chi^2_v = 1340/1237$. In this case only a single emissivity is required, where $q_1 = q_2 = 3.0 \pm 0.5$, while the disc abundance is consistent with solar. Given that the high black hole spin model only shows a marginal improvement in fit statistic ($\Delta\chi^2 = 11$ for three fewer degrees of freedom), then the claim of high black hole spin cannot be confirmed at a high confidence level, compared to the case where $a \sim 0$. Furthermore, if the Br2011 model is altered such that all three soft X-ray warm absorber zones fully cover the AGN, then this leads to a lower (and less constrained) value for the black hole spin, of $a = 0.35_{-0.10}^{+0.59}$, and is then formally consistent with the upper limit of $a < 0.31$ from the dual reflector model in P2011b.

The lower spin value may be due to the fact that the fully covering absorber adds greater spectral curvature to the model due to bound-free absorption, compared to the partial coverer. In the latter case, the absorption is diluted by an unabsorbed power law, reducing the amount of spectral curvature, while the breadth of the iron line profile can increase to compensate. Finally, we note that replacing the PEXMON model with a REFLIONX table for the distant reflector made little difference to any of the blurred reflection parameters and this appears unaffected by the parametrization of the distant reflection component.

We also attempted to recreate the maximal spin scenario subsequently presented by Rey2012, but applied to the model as constructed in P2011b and in this paper. Thus in this case we assumed that all three zones of the warm absorber in NGC 3783 fully cover the AGN as per P2011b and use the same warm absorber grids as in this paper, although the choice of a particular absorption model grid appears to not affect the reflection models. For ease of comparison, we also adopt the energy ranges used by Br2011 as above. We focus in particular on the Fe abundances, which Rey2012 suggest are critical for determining the blurred reflection parameters. The values for the disc reflector parameters from table 1 in Rey2012 are used, namely the iron abundances, spin, emissivities and break radii, all with the inner and outer radii set to the ISCO and $400R_g$, respectively. In summary we test three scenarios for the 2009 data: (i) $Z_{Fe,inner} = Z_{Fe,outer} = 3.3$ with near-maximal spin; (ii) $Z_{Fe,inner} = Z_{Fe,outer} = 1$ with $a = 0$; (iii) $Z_{Fe,inner} = 4.2$, $Z_{Fe,outer} = 1$ with near-maximal spin. These correspond closely to the models A, B and C respectively, as presented in table 1 of Rey2012. The KERRCONV model is used to blur the disc reflection spectra, while an unblurred low-ionization REFLIONX grid is maintained to model the distant reflector. Aside from the blurred reflection parameters as per Rey2012, the fit parameters are allowed to vary.

All three scenarios give a good fit to the data, with reduced chi-squared values of $\chi^2_v = 1300/1227, 1280/1227, 1284/1227$ for models (i), (ii) and (iii), respectively. Thus, all the spin and abundance scenarios are statistically acceptable, while the $a = 0$ and solar abundance case formally give the better fit. Allowing the disc parameters to vary for the solar abundance case then gives a constraint on the spin of $a < 0.45$ at 90 per cent confidence, while the disc emissivity is $q_1 = q_2 = 3.0 \pm 0.5$ and no break radius is required. Indeed the same solar abundance model when fitted over the energy ranges used in this paper also gives identical results and an equally good fit, with $\chi^2_v = 1414/1374$; see Table B4.

We also compare the fit focusing in on the Fe K band in Fig. 11, where the top panel shows the best-fitting dual reflector model

<figure><img src="image_19.png" /><figcaption>**Figure 11.** Upper panel: $v F_v$ 4–9 keV plot of the Patrick et al. (2011b) best-fitting model (with $a = 0$) to the 2009 NGC 3783 Suzaku data; note that the Fe K region is well modelled in the fit as is the broad red wing below 6.4 keV. Middle panel: residuals to the best-fitting dual reflector model, as shown in the upper panel with $a = 0$. Lower panel: residuals from the model with inner disc parameters as obtained by Reynolds et al. (2012b), i.e. with maximal spin, high emissivity and $Z_{Fe} > 3$. Both of the residual plots in the lower two panels show no noticeable difference in the Fe K region, thus it appears difficult to discriminate between the two scenarios.</figcaption></figure>

presented here (with $a = 0$) and the lower two panels show the data/model ratios for the scenarios (i) and (ii) above, with high spin and low spin, respectively. Clearly there is little difference in the residuals between the high-spin scenario with supersolar
abundances and the low-spin scenario with solar abundance. The
only marginal difference is the narrow core of the Fe Kα line at
6.4 keV is slightly overpredicted in the high-spin, high Fe abundance
scenario. This is in contrast to the plots shown in fig. 5 of Rey2012,
where the *a* = 0 scenario strongly overpredicts the red wing of
the line between 5 and 6 keV. This could be due to the fact that
the blurred reflector has a higher normalization in the high-spin
scenario, which when applied directly to the *a* = 0 case could
appear to overpredict the red wing, unless the normalization of the
reflector is refitted accordingly.

Finally, we note that if the RELLINE model is used instead of a
blurred reflection component, then a lower spin value is usually
preferred. For example, the upper limit on spin to NGC 3783 with
this model is *a* < 0.24 (also see Table 4). Indeed P2011b also
noted some tendency (although not statistically significant) for the
line to favour a retrograde black hole spin. The lower spin value
may be due to the fact that the model only fits the broad iron
line and not the reflected continuum, where the latter can often be
blurred to such an extent that it is hard to distinguish from the direct
continuum.

Thus the overall conclusion would appear to be that it is very
difficult to definitively determine the black hole spin in NGC 3783
with the present data, given the complexities of the models involved
and the deep warm absorber present in this AGN. For instance,
as discussed above, the construction of overall the model and the
warm absorber in particular can have an effect. In addition, the spin
value is indeed degenerate upon the iron abundance, as discussed
in Rey2012, and thus the high-spin cases always require high cen-
trally concentrated iron abundances. None the less a statistically
good fit is obtained with a simple solar abundance reflector and no
black hole spin. The evidence for a more complex picture with high
abundances, complex emissivity profiles and high spin would ap-
pear not to formally be required at high confidence, although neither
can the high-spin case be ruled out at present.

4.3.5 Truncation of the disc

As can be seen from Table 4 and Fig. 9, the majority of AGN
in this sample do not feature strong emission from the very inner
regions of the accretion disc, both the emissivity index and spin
of the central BH take typically low values. This suggests that
the dominant regions producing the typical broad iron line profile
are regions close to but more distant from the central BH than has
been estimated in many analyses (Reynolds, Brenneman & Garofalo
2005; Brenneman & Reynolds 2006; Miniutti et al. 2007; Br2011;
Reynolds et al. 2011b), originating at typically tens of R<sub>g</sub> and hence
with a significant amount of flux present in the blue wing of the
line profile as opposed to the red wing. The RELLINE fits in Table 4
are under the assumption that the inner radius of the accretion disc
extends down the ISCO (i.e. R<sub>ISCO</sub>), if the majority of the line profile
originates from the outer regions of the disc, it is plausible that in
some cases the accretion disc may be truncated at a few to tens of
R<sub>g</sub>. For example, Lobban et al. (2010) suggest a truncated accretion
disc in NGC 7213, stating a lack of a significant broad component
in the Fe K region and weak reflection. If the inner edge of the
accretion disc does not extend down to the ISCO, it would make the
determination of SMBH spin through spectral fitting very difficult.
Essentially at R<sub>in</sub> > 9 R<sub>g</sub> the spin could take any value -0.998 <
*a* < 0.998 with the disc truncated at any R<sub>in</sub> with little difference
upon the relativistic line profile.

4.3.6 Alternative mechanisms

Recent work by Tatum et al. (2012) suggests that an alternative
mechanism to reflection from the inner regions of the accretion
disc is emission from a Compton-thick disc wind based upon a
disc wind model by Sim et al. (2010). The authors take the clean-
est sources possible, i.e. the ‘bare’ Seyfert sample from Patrick
et al. (2011a) and assuming a relatively face-on viewing angle
whereby only the scattered light from the wind is observed rather
than any absorption features with a more edge-on viewing angle.
The line profiles are therefore subject to velocity broadening due
to Doppler velocity shear across the wind and Compton downscat-
tering of the Fe Kα flux; these can combine to imitate a broad-
line profile from reflection off the inner regions of the accretion
disc. Good fits are made to the broad-band spectra for this model
without the requirement for any further broadened emission from
reflection off the inner regions of the disc. In this scenario, the
full Fe K line profile is reproduced with solar iron abundances at
typically tens to hundreds of R<sub>g</sub>; however, in some objects an ad-
ditional cold neutral reflector and neutral Fe Kα line component
are still required in order to model the Fe K edge and hard X-ray
excess.

While the disc wind model alone can start replicate many of
the features in the broad-band spectrum, it is likely that the true
scenario is a combination of absorption, reflection and scattered
components off both the disc and a wind, a scenario which may not
be resolved with current X-ray observatories without calorimeter
resolution spectra in the Fe K band. It is, however, interesting to
note that the tentative bimodality of the broad-line EWs in this
sample (Fig. 9) may represent such a scenario whereby a fraction
of the weaker observed broad lines are as a result of disc wind
geometries. Meanwhile objects which display stronger broad lines
(EW $\gtrsim$ 150 eV) may be the only objects in which we can see the
inner tens of R$_g$ of the disc. It must be stressed, however, that the
apparent (albeit weak) bimodal nature of the EWs in this sample
may simply be due to insufficient statistics.

4.4 Distant reflection

The use of the HXD instrument on Suzaku and BAT on-board Swift
allows us to examine the hard X-ray spectra of the objects in this
sample and to appropriately parametrize the distant reflection com-
ponent. This may arise, for example, from the reflection of contin-
uum X-rays off the cold (T < 10⁶ K) outer regions of the accretion
disc or via a parsec-scale torus.

The majority of AGN in this sample show evidence for a reflec-
tion component; only 7/46 (see Table 5) do not require the addition
of the unblurred *REFLIONX* model (3C 111, IRAS 13224–3809, MR
2251–178, Mrk 79, NGC 7314 and PG 1211+143). Neither are
these objects best described with a high column density partially
covering absorbing zone with N_H ~ 10^24 cm^-2 which can replicate
a hard X-ray excess to some extent, i.e. there is no apparent hard ex-
cess in these objects. Table B5 also indicates that the large majority
of AGN in this sample do feature excess emission in the 15–50 keV
region over the extrapolated 2–10 keV intrinsic power law. A num-
ber of the objects in the sample feature particularly strong reflection
with 15–50 keV reflector flux F_reflector $\gtrsim$ 3 × 10^−11 erg cm^−2 s^−1,
namely IC 4329A, MCG+8-11-11, NGC 3227, NGC 3783, NGC
4151 and NGC 5506. In addition to this, a large number of the AGN
in this sample feature particularly hard X-ray spectra, i.e. those with
a high hardness ratio F_15–50 keV/F_2–10 keV $\gtrsim$ 3: 3C 445, Mrk 279,
NGC 1365, NGC 3227 (Obs 2, 4 and 6), NGC 3516 (Obs 1) and
<figure><img src="image_20.png" /><figcaption>**Figure 12.** The distribution of reflection fractions for each observation in the sample with values obtained from Table B5 whereby the fraction is the ratio of the 15–50 keV reflected flux to the 15–50 keV continuum flux (i.e. full model minus reflected flux). Note that the majority of AGN feature reflection fractions between 0 and 0.7. The final bin from 1.1 upwards contains only three observations of AGN with $R_{15-50} = 1.6, 3.5$ and $7.2$. $R_{15-50} = 0.8$ is equivalent to a $R = 1$ PEXRAV versus a simple unabsorbed POWERLAW.</figcaption></figure>

NGC 4151 (see Table B5):

$$R_{15-50} = \frac{\text{Reflected flux}}{\text{Full model flux} - \text{Reflected flux}} \quad (1)$$

Taken from values in Table B5 we also calculate a reflection fraction over the 15–50 keV range using equation (1); note that this $R_{15-50}$ is not the same as the reflection fraction R included in models such as PEXRAV (Magdziarz & Zdziarski 1995). For ease of comparison, we calculate the equivalent $R_{15-50}$ value for an $R = 1$ PEXRAV versus a simple unabsorbed $\Gamma = 2$ POWERLAW; this yields $R_{15-50} \sim 0.8$. The reflection fraction is particularly high in eight observations in the sample and four objects (MCG–02-14-009, NGC 3227, NGC 3783 and NGC 4151). In these objects the reflector flux in the 15–50 keV band contributes approximately half of the total 15–50 keV flux; however, this appears to bear no correlation with properties such as covering fraction although each of these four objects does feature relatively high hardness ratios (ratio of 15–50 to 2–10 keV flux). The majority of AGN, however, feature reflection fractions fitting a smooth distribution between $R_{15-50} = 0$ and $R_{15-50} = 0.7$ (see Fig. 12). The measured strength of the reflection component can be somewhat degenerate with the method in which the partial coverer is modelled. However, the reflection continuum below 10 keV can help to ensure that the correct amount of hard X-ray flux is produced by REFLIONX by measuring the strength of the narrow 6.4-keV core, for an appropriate iron abundance, the self-consistent reflection strength is then modelled above 10 keV. Any remaining residuals > 10 keV must then be due to a high column density partial coverer. That is, the strength of the narrow 6.4-keV core can give a reasonable estimate of the contribution of the reflector above 10 keV.

A significant number of AGN in this sample are fitted very well assuming a simple solar iron abundance, i.e. $Z_{Fe} = 1.0$ when allowed to vary as a free parameter within REFLIONX. Although the narrow Fe Kα core is sufficiently strong in at least nine objects that further neutral iron emission is required from material distant to the central SMBH, e.g. the BLR in addition to reflection off the torus. Four objects strongly require subsolar iron abundance (IC 4329A, NGC

3227, NGC 5506 and SWIFT J2127.4+5654) while 4/39 statistically prefer a slight supersolar iron abundance (typically $Z_{Fe} \lesssim 3$). This suggests that the hypothesis of solar abundances throughout the disc and central engines of these AGN is a reasonable assumption in contrast to supersolar $Z_{Fe}$ based upon inner disc reflection (e.g. Br2011; Fabian et al. 2012). The analysis of the 46 objects in this sample indicates that the reflection in an overwhelming majority of the Seyfert 1 type AGN in the Suzaku archive is well described by reflection of a cold, distant, neutral material with solar abundances throughout, also see Nandra & Pounds (1994) and Rivers, Markowitz & Rothschild (2011a) for similar findings regarding the recurrent presence of the Compton hump. We note that in higher 2–10 keV luminosity AGN we find that the EW of the narrow Fe Kα emission line is low in comparison to other lower luminosity AGN, although the sample in this paper lacks the sufficient statistics to support the evidence for the X-ray Baldwin effect as suggested by Jiang, Wang & Wang (2006) and Fukazawa et al. (2011).

## 4.5 Warm absorbers and partial covering

The way in which absorbing zones are modelled in X-ray spectra can have a significant effect upon the Fe K region and the estimation of properties relating to the central SMBH and the surrounding accretion disc. Within this Suzaku sample, a large proportion of AGN feature complex absorbers, requiring one or more zones of an XSTAR grid. Only 12/46 (26 per cent) of objects in this sample can be considered ‘bare’ for the purposes of this paper – featuring no statistically significant additional absorption zones in addition to the neutral Galactic column, these are 3C 390.3, Ark 120, Fairall 9, MCG–02-14-009, Mrk 110, Mrk 335, Mrk 359, NGC 3147, NGC 7213, NGC 7469 and RBS 1124. A few objects in the sample (6/46, 9 per cent) feature an additional neutral zone of absorbing gas at the redshift of the object, while the remaining 27/46 (59 per cent) all require the application of complex warm (i.e. ionized) zones of gas to model the broad-band spectrum.

Just over one-third of the sample (16 AGN) also statistically require a partially covering geometry (i.e. 35 per cent of the total sample, Table 5). In this scenario one of the absorbing zones of gas (typically high column $N_H \gtrsim 5 \times 10^{23}$ cm$^{-2}$) partially obscures the nucleus in addition to one or more lower column density fully covering absorbing zone. The majority of the partial covering models in this sample have a sufficiently high column density such that their predominant effect is to supplement and increase the hard X-ray flux. The distribution of covering fractions for the partial covering fits here covers the full range from low to high covering fractions (Fig. 13).

We note that only single-layer partial covering geometries are used (where formally required) in this analysis since multiple layers can be somewhat ambiguous and care must be taken to ensure that layers are not added on an ad hoc basis until all features are removed from the spectrum. None of the objects in this sample requires more than a single layer of partial covering in order to obtain an acceptable fit to the broad-band data.

Partial covering scenarios in some previous analyses have been used to model spectral curvature in the Fe K region which may otherwise be attributed to relativistic line emission, e.g. MCG–6-30-15 by Miller et al. (2009). However, careful examination of the effects of high column partial coverers such as those used here suggests that the measured strength of broad-line emission in the Fe K region is simply reduced (i.e. lower EW) while the estimated accretion disc parameters and BH spin estimates remain relatively unchanged (for example MCG–06-30-15 in P2011b; Section 3.3.1). During
<figure><img src="image_21.png" /><figcaption>**Figure 13.** The distribution of partial covering fractions. Note that the full range is covered with a relatively even distribution.</figcaption></figure>

the analysis of this sample we have also noted that the application of high column density partial covering scenarios in fact has some bearing upon the iron abundance of the reflector derived from reflection models such as REFLIONX (or indeed PEXMON). Since the partial coverer produces additional flux at hard X-ray energies, it is possible that the reflection continuum is subsequently underpredicted and the iron abundance is increased to compensate for the lack of narrow Fe Kα core flux. However, the majority of the objects here in which we require additional narrow Fe Kα emission through the use of an additional narrow Gaussian do not feature partial covering and therefore it seems likely that the additional narrow line flux in these particular objects originates from distant material, as opposed to being a consequence of improper modelling of the spectrum above 10 keV.

## 4.6 Inner reflection versus partial covering

The baseline model constructed in the main models of this paper makes use of a high column partial coverer to account for any additional hard X-ray flux which may be present in the X-ray spectra of these AGN. An alternate scenario is to use a blurred reflection component from the inner regions of the disc in addition to an unblurred reflector from the outer regions of the disc which can provide a means of supplementing the total hard X-ray flux at >10 keV. As noted in Section 3.4, this scenario can provide a good description of the broad-band spectrum for MCG-06-30-15 and NGC 5506 whilst retaining relatively typical accretion disc parameters, i.e. low to moderate emissivity index and inclination, similar to those obtained from an analysis of the broad Fe Kα line profile (see Section 3.3 and Table 4).

The fit to the remaining objects (Mrk 766, NGC 1365, NGC 3516, NGC 3783 and NGC 4051) is worse without a partial covering geometry. This may be due to the inability of the inner reflector geometry to successfully describe the long-term variability (e.g. variability in spectral curvature) of these AGN; all of which are noted to have varied between each of the observations analysed here. In each of these AGN, the disc parameters are either poorly constrained or forced to extreme values, e.g. in order to describe the broad-band spectrum and long-term variability of NGC 4051, the emissivity of the disc is increased to $q = 6.1_{-0.1}^{+0.3}$ and spin to near maximal $a > 0.99$, while producing an overall worse fit. This suggests that emission is required to be very centrally concentrated

with the inner reflector proving the dominant component in the broad-band model. For example, the inner reflector for 2005 observation of NGC 4051 has 15–50 keV flux ~8.8 times higher than the outer reflector [$F_{2005\text{inner}} = (1.49_{-0.03}^{+0.02}) \times 10^{-11} \text{ erg cm}^{-2} \text{ s}^{-1}$ versus $F_{2005\text{outer}} = (0.17_{-0.02}^{+0.01}) \times 10^{-11} \text{ erg cm}^{-2} \text{ s}^{-1}$]. Comparing this to the alternative (i.e. with partial covering explaining the long-term spectral variability; Table B4), the inner reflector 15–50 keV flux is significantly reduced when partial covering is invoked: $F_{2005\text{inner}} = (0.29_{-0.03}^{+0.03}) \times 10^{-11} \text{ erg cm}^{-2} \text{ s}^{-1}$ compared to $F_{2005\text{outer}} = (0.37_{-0.05}^{+0.08}) \times 10^{-11} \text{ erg cm}^{-2} \text{ s}^{-1}$.

We find here that in the majority of cases, the dual reflector scenario does not provide a reasonable alternative to a partial covering geometry particularly in objects which feature significant long-term spectral variability (see Table B4). NGC 1365 is very poorly fitted with $\chi_v^2 \sim 2.2$ above 2 keV and $\chi_v^2 \sim 5.1$ over the 0.6–100 keV range; NGC 3227 and NGC 3516 also feature poor fits with $\chi_v^2 \sim 1.2$ and $\chi_v^2 \sim 1.8$ respectively when fitted without partial covering. It should be noted that many of the iron line parameters in Tables B4 are poorly constrained; this is due to the interplay between the inner reflector and outer reflector (and/or partial covering) at hard X-ray energies and the COMPTT component at soft X-ray energies.

## 5 CONCLUSIONS

Based upon an analysis of all publicly available Suzaku observations of Seyfert 1 AGN with observations longer than 50 ks and greater than 30 000 XIS counts, we conclude the following.

(i) The majority (59 per cent) of AGN in this sample feature complex warm absorption which has a significant effect upon the Fe K region and any accretion disc parameters derived from it. The use of the full 0.6–100.0 keV broad-band data is therefore essential prior to any attempt to use relativistic line profile models as a diagnostic for the inner regions of the accretion disc. The mean photon index of the 46 objects on the sample is $\Gamma = 1.82 \pm 0.03$.

(ii) Absorptions in the Fe K region due to highly ionized gas producing absorption features from Fe XXV and Fe XXVI are relatively common in AGN (30 per cent), most of which (71 per cent) are outflowing at high velocities. While a large fraction of the detected highly ionized winds are outflowing, there may be a larger number of low-velocity winds which are not detected due to the possible presence of ionized Fe XXV and Fe XXVI emission lines. The additional curvature added to the region through modelling with an appropriate XSTAR grid, while subtle, has a notable effect upon the strength of any broad residuals which may remain below 6.4 keV and be interpreted as strong relativistic emission.

(iii) A partial covering geometry is required in 35 per cent of all objects in the sample. These high column density zones primarily affect the hard X-ray spectrum above 7 keV although reducing the strength of broad residuals in the Fe K region rather than removing them entirely.

(iv) Narrow ionized emission in the Fe K region from Fe XXV and Fe XXVI are relatively common in these AGN, featuring in 24/46 and 18/46 of objects, respectively. Of these AGN, 10/46 feature both Fe XXV and Fe XXVI emission. These lines are found to be much more common compared to an XMM-Newton survey by Nandra et al. (2007) despite possible interplay with the blue wing of more sophisticated relativistic line emission models which could reduce the number of narrow-line detections.

(v) Examining the Fe K region after a complete modelling of the broad-band 0.6–100.0 keV spectrum and all required absorption
zones yields a range of weak to moderate strength broad residuals below 6.4 keV. We find that 26/46 (56 per cent) of the objects in this sample require some degree of relativistic line emission in the Fe K region at 90 per cent confidence and 23/46 (50 per cent) at >99.5 per cent confidence.

(vi) These broad residuals are well fitted with the RELLINE model and yield an average broad-line strength of EW = 96±10 eV for the total of 26 objects. The line energy and $\sigma_{width}$ of the broad residuals when modelled with a Gaussian are consistent with Nandra et al. (2007).

(vii) We estimate an average emissivity index of the accretion disc of $q = 2.4 \pm 0.1$, suggesting that emission from the accretion disc responsible for relativistic lines is not extremely centrally concentrated when purely the line profile in the Fe K region is used as a diagnostic. The majority of the line flux therefore occurs from the blue wing of the line profile with emission being insufficiently close to $R_{ISO}$ as to redshift a significant proportion of the X-ray flux into a strong red wing. We also measure an average disc inclination of $i = 33^{\circ} \pm 2^{\circ}$ and inner radius of emission $R_{in} = (21 \pm 6) R_g$.

(viii) With the assumption that the inner radius of the accretion disc ($R_{in}$) extends down to the ISO ($R_{ISO}$), loose constraints upon the SMBH spin parameter $a$ can be made. The relativistic line emission profiles are sufficiently distinguished in 11/46 objects to place upper or lower bounds on the spin. After a broad-band analysis we make the following estimates: Ark 120, $a < 0.94$; Fairall 9, $a = 0.60^{+0.19}_{-0.63}$; MCG-02-14-009, $a < 0.88$; MCG-05-23-16, $a < 0.50$; MCG-06-30-15, $a = 0.49^{+0.20}_{-0.12}$; Mrk 79, $a < 0.80$; Mrk 335, $a = 0.70^{+0.12}_{-0.01}$; NGC 3516, $a < 0.30$; NGC 3783, $a < 0.24$; NGC 7469, $a = 0.69^{+0.09}_{-0.09}$ and SWIFT J2127.4+5654 with $a = 0.70^{+0.10}_{-0.14}$. Under the assumption that $R_{in} = R_{ISO}$, a maximally rotating SMBH is ruled out in each of these 11 objects.

## ACKNOWLEDGMENTS

This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). We acknowledge the use of public data from the Swift data archive. We thank Laura Brenneman and Chris Reynolds for discussions regarding the Suzaku spectrum of NGC 3783. We would also like to thank the referee for their helpful comments.

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# APPENDIX A: SELECTED INDIVIDUAL OBJECTS

## A1 Fairall 9

The Fe K region of the 'bare' Seyfert Fairall 9 has been well studied (Schmoll et al. 2009; Emmanoulopoulos et al. 2011; Patrick et al. 2011a; P2011b); here a simultaneous analysis of both the 2007 and 2010 observations provides a good fit to the data, simply allowing the normalization of the components to vary. In line with each of the previous analyses, we find an emissivity $q = 2.9_{-0.4}^{+0.5}$ although a somewhat more poorly constrained spin parameter $a = 0.60_{-0.62}^{+0.19}$, i.e. consistent with zero spin in this analysis of both Fairall 9 Suzaku observations.

## A2 Mrk 205

The best-fitting model for Mrk 205 presented here features partial covering to account for additional flux at X-ray energies >10 keV. The subsequent addition of a broad Gaussian or RELLINE component has little effect upon the overall fit (an improvement of $\Delta\chi^2 \sim 4$) due to the spectral curvature introduced as a result of a partial coverer with column density $N_H = (5.1_{-2.5}^{+5.5}) \times 10^{23} \text{ cm}^{-2}$, ionization $\log(\xi) = 2.8_{-0.5}^{+0.7}$ erg cm s$^{-1}$ and covering fraction $C_{frac} = 13$ per cent. However, this AGN can be equally well described with a very broad iron line with EW = $254_{-59}^{+72}$ eV and an increase of $\Delta\chi^2 \sim +23$ when the RELLINE component is removed and the model refitted without a partial coverer in place. This yields a relatively high emissivity index of $q = 3.4_{-0.5}^{+1.4}$, an inclination of $i = 30^{\circ}_{-9}$ and a lower limit placed upon the spin parameter $a > 0.1$.

## A3 NGC 3227

The six observations of NGC 3227 amount to nearly 500 000 2–10 keV counts and a relatively simple model is formed to describe

each component and the variations between observations. The best-fitting model for NGC 3227 consists of a high-column partial covering component of column $N_H = (2.9_{-0.1}^{+0.1}) \times 10^{23} \text{ cm}^{-2}$ with a variable covering fraction of $C_{frac} \sim 32–89$ per cent in addition to a single warm absorbing zone and both hard and soft excesses fitted with RELLIONX and COMP TT, respectively. Examining the Fe K region, there are clear absorption lines due to Fe xxv and Fe xxvi and small residuals indicative of weak to moderate emission from the inner regions of the accretion disc (with EW generally higher in a lower continuum flux spectrum; also noted by Fukazawa et al. 2011). A good fit to each of the six observations is found simply by letting the strength of the RELLIONX and COMP TT to vary as well as the covering fraction of the partial coverer. All absorber properties such as ionization and column density are tied between observations other than the covering fraction and ionization of the partial coverer which is required to vary between log $\xi \sim 0.50$ and 1.53 with each observation. Using the RELLINE model to account for the broad residuals with parameters tied (but again allowing normalization to vary) yields an improved fit to the data with $\chi^2 = 4465.6/4189$. The RELLINE model yields a relatively typical emissivity of $q = 2.7_{-0.4}^{+0.5}$ and an inclination of $i = 33^{\circ}_{-2}$ and $R_{in} = 11_{-6}^{+3} R_g$ (Table 4 and Fig. 7).

## A4 NGC 3516

The two observations of NGC 3516 differ in their shape significantly (Markowitz et al. 2008), the 2005 Suzaku observation 2–10 keV flux is a factor of 1.8 higher than in the 2009 observation. Here we have formed a model in which a good fit is found to both observations, allowing for changes in the absorber/partial coverer properties and strength of reflection between data sets, although the basic geometry is maintained and a good overall fit is found. As noted in P2011b and Turner et al. (2011), the 2009 observation showed no strong indication of a broad red wing; however, the Markowitz et al. (2008) analysis of the earlier 2005 data do suggest the presence of such a feature. The 2005 observation is more absorbed than the 2009 observation (i.e. $C_{frac} = 83$ per cent compared to 18 per cent in the 2009 observation), yet it has a much higher continuum flux level throughout the spectrum above ~2 keV (Fig. 7). This simultaneous analysis yields consistent results with previous work, retrieving the broad feature found by Markowitz et al. (2008) in the 2005 data. Fitting a RELLINE component to both data sets with all parameters (other than normalization) tied suggests a fairly typical and relatively weak broad line with EW = $58_{-9}^{+9}$ eV and significantly weaker EW = $14_{-2}^{+2}$ eV in the 2005 and 2009 observations, respectively. An upper limit to the spin parameter is found $a < 0.30$ and inclination $i < 41^{\circ}$ at a disc emissivity of $q = 3.1_{-0.2}^{+0.4}$.

## A5 NGC 4051

The three Suzaku observations of NGC 4051 (as used in Lobban et al. 2011) included in this analysis vary significantly (see Figs 6 and 7). In particular, in the 2005 observation (OBSID: 700004010) the source dips into an extended period of low flux versus the two 2008 observations which show the object in a period of high flux ($F_{2-10\text{keV}} 2008 \sim 3.8 \times F_{2-10\text{keV}} 2005$; see Fig. 7 and Table B5). Similarly to Lobban et al. (2011), we can successfully describe each observation and the long-term spectral variability with a partial covering scenario whereby parameters such as the column density and ionization of the absorbing zones of gas remain approximately constant ($N_H \sim 9 \times 10^{22} \text{ cm}^{-2}$, over these time-scales at least). The differences in the broad-band spectrum of each observation can be accounted for simply by allowing the normalization
of the intrinsic power law, soft excess and distant reflection component to vary, in addition to the covering fraction of the partially covering absorption zone. Here we find covering fractions of 67, 11 and 27 per cent for observations 1, 2 and 3 respectively albeit with a much flatter intrinsic power law (Γ ~ 1.88 here versus Γ ~ 2.49 in Lobban et al. 2011); however, this is likely due to the treatment of the soft excess and reflection components. Here (for consistency with the analysis of other objects in the sample) we account for the soft excess with a COMP TT component which is akin to a second soft POWERLAW, this could in part explain the discrepancies between the two different intrinsic power-law components.

Similarly to Lobban et al. (2011), we find strong evidence for blueshifted absorption in the Fe K region indicative of an outflowing highly ionized zone of gas. When described as such, we find an outflow velocity of 5800$^{+1400}_{-1300}$ km s$^{-1}$ in each observation, consistent with Lobban et al. (2011). Both the Lobban et al. (2011) and the baseline models in this analysis describe the spectral variability with absorption-dominated models. Replacing the partial coverer with a reflection component representing emission from the inner regions of the accretion disc as an alternate means of accounting for the hard excess and spectral curvature (i.e. a dual reflector) yields a fit worse by $\Delta\chi^2 \sim +137$ for four fewer degrees of freedom.

Parameters such as SMBH spin and the emissivity index of the disc are forced to high values, i.e. $a \sim 0.996$ and $q = 6.1^{+0.3}_{-0.1}$. This is in order to smooth the reflection continuum to the extent to which it can successfully account for the long-term spectral variability between observations, i.e. accounting for both the hard excess and subtle continuum curvature changes. The partial covering scenario is therefore preferred both statistically and in terms of physical implications, i.e. extreme parameters and relativistic blurring are not required which would otherwise significantly deviate from the sample norm. Note that there is still a evidence for an highly ionized outflow in the Fe K region, regardless of the application of a dual reflector or partial covering based model.

Based upon this, it is clear that the long-term spectral variability of NGC 4051 cannot be produced purely by varying the reflected flux in a reflection-dominated model; instead a partial covering scenario must be invoked to some extent in order to accurately reproduce the differences between each of the three Suzaku observations. Reintroducing a partial covering geometry (in addition to a dual reflector; Section 3.4) restores a fit similar to the baseline model. It is, therefore, perhaps more feasible than the broad-band spectrum and variability of NGC 4051 (in addition to other AGN) is primarily a result of variations in covering fraction in an absorption and not reflection-dominated spectrum.

APPENDIX B:

<table><caption>Table B1. Summary of observations for the objects in the sample. The XIS count rates listed are per XIS. We use BAT data from the 58-month BAT catalogue (Baumgartner et al. 2010).</caption><thead><tr><th>Object</th><th>Mission</th><th>Instrument</th><th>Date</th><th>Exposure (s)</th><th>Count rate</th><th>Flux<sup>a</sup></th><th>ObsID</th><th>No. counts</th></tr></thead><tbody><tr><td rowspan="4">1H 0419-577</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007-07-25</td><td>205 863</td><td>1.251 ± 0.002</td><td>1.75</td><td rowspan="2">702041010</td><td>519 055</td></tr><tr><td>HXD</td><td>142 600</td><td>0.052 ± 0.002</td><td>2.93</td><td>45 303</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2010-01-16</td><td>122 835</td><td>0.866 ± 0.02</td><td>1.40</td><td rowspan="2">704064010</td><td>217 440</td></tr><tr><td>HXD</td><td>104 900</td><td>0.028 ± 0.001</td><td>2.18</td><td>22 240</td></tr><tr><td>Swift</td><td>BAT</td><td>-</td><td>-</td><td>(2.4 ± 0.3) × 10<sup>-4</sup></td><td>1.71</td><td>-</td><td>940</td></tr><tr><td rowspan="3">3C 111</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2008-08-22</td><td>122 378</td><td>0.610 ± 0.002</td><td>1.95</td><td rowspan="2">703034010</td><td>152 164</td></tr><tr><td>HXD</td><td>101 900</td><td>0.068 ± 0.002</td><td>3.29</td><td>36 150</td></tr><tr><td>Swift</td><td>BAT</td><td>-</td><td>-</td><td>(10.2 ± 0.3) × 10<sup>-4</sup></td><td>7.43</td><td>-</td><td>-</td></tr><tr><td rowspan="6">3C 120</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2006-02-09</td><td>41 932</td><td>3.082 ± 0.005</td><td>4.63</td><td rowspan="2">700001010</td><td>389 949</td></tr><tr><td>HXD</td><td>31 870</td><td>0.099 ± 0.004</td><td>6.24</td><td>13 996</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2006-02-16</td><td>42 555</td><td>2.464 ± 0.004</td><td>4.01</td><td rowspan="2">700001020</td><td>309 300</td></tr><tr><td>HXD</td><td>34 540</td><td>0.144 ± 0.005</td><td>5.72</td><td>21 832</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2006-02-23</td><td>40 907</td><td>2.53 ± 0.004</td><td>4.04</td><td rowspan="2">700001030</td><td>312 550</td></tr><tr><td>HXD</td><td>36 200</td><td>0.110 ± 0.004</td><td>6.07</td><td>15 360</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2006-03-02</td><td>40 905</td><td>2.351 ± 0.004</td><td>3.96</td><td rowspan="2">700001040</td><td>290 680</td></tr><tr><td>HXD</td><td>37 870</td><td>0.093 ± 0.003</td><td>5.59</td><td>14 533</td></tr><tr><td>Swift</td><td>BAT</td><td>-</td><td>-</td><td>(8.5 ± 0.2) × 10<sup>-4</sup></td><td>5.82</td><td>-</td><td>-</td></tr><tr><td rowspan="3">3C 382</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007-04-27</td><td>130 580</td><td>2.596 ± 0.003</td><td>4.05</td><td rowspan="2">702125010</td><td>683 288</td></tr><tr><td>HXD</td><td>114 300</td><td>0.097 ± 0.002</td><td>5.11</td><td>47 714</td></tr><tr><td>Swift</td><td>BAT</td><td>-</td><td>-</td><td>(7.6 ± 0.2) × 10<sup>-4</sup></td><td>5.11</td><td>-</td><td>-</td></tr><tr><td rowspan="3">3C 390.3</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2006-12-14</td><td>179 800</td><td>1.831 ± 0.003</td><td>3.10</td><td rowspan="2">701060010</td><td>333 573</td></tr><tr><td>HXD</td><td>92 060</td><td>0.096 ± 0.003</td><td>5.81</td><td>37 078</td></tr><tr><td>Swift</td><td>BAT</td><td>-</td><td>-</td><td>(9.09 ± 0.18) × 10<sup>-4</sup></td><td>6.82</td><td>-</td><td>-</td></tr><tr><td rowspan="3">3C 445</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007-05-25</td><td>139 769</td><td>0.159 ± 0.001</td><td>0.70</td><td rowspan="2">702056010</td><td>48 098</td></tr><tr><td>HXD</td><td>109 500</td><td>0.049 ± 0.002</td><td>2.69</td><td>37 749</td></tr><tr><td>Swift</td><td>BAT</td><td>-</td><td>-</td><td>(3.7 ± 0.2) × 10<sup>-4</sup></td><td>2.35</td><td>-</td><td>-</td></tr><tr><td rowspan="3">4C 74.26</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007-10-28</td><td>91 583</td><td>1.493 ± 0.003</td><td>3.13</td><td rowspan="2">702057010</td><td>276 179</td></tr><tr><td>HXD</td><td>87 340</td><td>0.084 ± 0.002</td><td>4.00</td><td>34 810</td></tr><tr><td>Swift</td><td>BAT</td><td>-</td><td>-</td><td>(4.6 ± 0.2) × 10<sup>-4</sup></td><td>3.37</td><td>-</td><td>-</td></tr><tr><td rowspan="3">Ark 120</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007/04/01</td><td>100 864</td><td>1.896 ± 0.003</td><td>3.05</td><td rowspan="2">702014010</td><td>384 821</td></tr><tr><td>HXD</td><td>89 470</td><td>0.114 ± 0.003</td><td>3.46</td><td>51 795</td></tr><tr><td>Swift</td><td>BAT</td><td>-</td><td>2453 000</td><td>(6.9 ± 0.4) × 10<sup>-4</sup></td><td>4.89</td><td>-</td><td>1690</td></tr></tbody></table>
<table><caption>Table B1 – continued</caption><thead><tr><th>Object</th><th>Mission</th><th>Instrument</th><th>Date</th><th>Exposure (s)</th><th>Count rate</th><th>Flux<sup>a</sup></th><th>ObsID</th><th>No. counts</th></tr></thead><tbody><tr><td rowspan="2">Ark 546</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007-06-26</td><td>99 978</td><td>2.277 ± 0.003</td><td>1.84</td><td rowspan="2">702117010</td><td>458 819</td></tr><tr><td>HXD</td><td>81 330</td><td>0.021 ± 0.002</td><td>1.54</td><td>15 343</td></tr><tr><td rowspan="6">Fairall 9</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007-06-07</td><td>167 814</td><td>1.718 ± 0.002</td><td>2.32</td><td rowspan="2">702043010</td><td>581 331</td></tr><tr><td>HXD</td><td>127 310</td><td>0.089 ± 0.002</td><td>2.97</td><td>46 809</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2010-08-26</td><td>229 296</td><td>1.780 ± 0.002</td><td>2.17</td><td rowspan="2">705063010</td><td>742 007</td></tr><tr><td>HXD</td><td>162 200</td><td>0.039 ± 0.002</td><td>3.51</td><td>65 230</td></tr><tr><td>Swift</td><td>BAT</td><td>–</td><td>–</td><td>(4.7 ± 0.2) × 10<sup>-4</sup></td><td>3.34</td><td>–</td><td>1619</td></tr><tr><td rowspan="6">IC 4329A</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007-08-01</td><td>25 453</td><td>5.212 ± 0.010</td><td>10.64</td><td rowspan="2">702113010</td><td>266 796</td></tr><tr><td>HXD</td><td>20 050</td><td>0.289 ± 0.006</td><td>15.96</td><td>11 647</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007-08-06</td><td>30 623</td><td>6.138 ± 0.010</td><td>12.58</td><td rowspan="2">702113020</td><td>377 880</td></tr><tr><td>HXD</td><td>24 080</td><td>0.340 ± 0.005</td><td>17.97</td><td>15 349</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007-08-11</td><td>26 896</td><td>5.554 ± 0.010</td><td>11.89</td><td rowspan="2">702113030</td><td>300 624</td></tr><tr><td>HXD</td><td>22 110</td><td>0.345 ± 0.006</td><td>18.77</td><td>15 541</td></tr><tr><td rowspan="6">IRAS 13224–3809</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007-08-16</td><td>24 219</td><td>5.261 ± 0.010</td><td>10.88</td><td rowspan="2">702113040</td><td>256 495</td></tr><tr><td>HXD</td><td>18 750</td><td>0.300 ± 0.006</td><td>16.47</td><td>11 923</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007-08-20</td><td>24 026</td><td>3.221 ± 0.008</td><td>7.03</td><td rowspan="2">702113050</td><td>156 141</td></tr><tr><td>HXD</td><td>17 520</td><td>0.242 ± 0.006</td><td>13.69</td><td>9755</td></tr><tr><td rowspan="2">Suzaku</td><td>BAT</td><td>–</td><td>–</td><td>(26.8 ± 0.3) × 10<sup>-4</sup></td><td>19.02</td><td>–</td><td>–</td></tr><tr><td>XIS</td><td rowspan="2">2007-01-26</td><td>197 938</td><td>0.085 ± 0.001</td><td>0.06</td><td rowspan="2">701003010</td><td>39 148</td></tr><tr><td>HXD</td><td>158 500</td><td>0.004 ± 0.002</td><td>0.015</td><td>86 214</td></tr><tr><td rowspan="2">MCG-02-14-009</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2008-08-28</td><td>142 152</td><td>0.216 ± 0.001</td><td>0.43</td><td rowspan="2">703060010</td><td>63 436</td></tr><tr><td>HXD</td><td>120 028</td><td>0.017 ± 0.002</td><td>0.61</td><td>40 150</td></tr><tr><td rowspan="2">MCG-02-58-22</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2009-12-02</td><td>138 969</td><td>2.921 ± 0.003</td><td>4.87</td><td rowspan="2">704032010</td><td>817 420</td></tr><tr><td>HXD</td><td>97 980</td><td>0.163 ± 0.002</td><td>8.73</td><td>44 009</td></tr><tr><td rowspan="2">Suzaku</td><td>BAT</td><td>–</td><td>–</td><td>(9.8 ± 0.2) × 10<sup>-4</sup></td><td>7.48</td><td>–</td><td>–</td></tr><tr><td>XIS</td><td rowspan="2">2005-12-07</td><td>95 677</td><td>2.822 ± 0.003</td><td>8.93</td><td rowspan="2">700002010</td><td>815 975</td></tr><tr><td>HXD</td><td>79 690</td><td>0.313 ± 0.003</td><td>14.52</td><td>55 913</td></tr><tr><td rowspan="2">Suzaku</td><td>BAT</td><td>–</td><td>–</td><td>(19.8 ± 0.2) × 10<sup>-4</sup></td><td>14.27</td><td>–</td><td>4526</td></tr><tr><td>XIS</td><td rowspan="2">2006-01-09</td><td>143 196</td><td>2.862 ± 0.003</td><td>4.38</td><td rowspan="2">700007010</td><td>1240 090</td></tr><tr><td>HXD</td><td>118 900</td><td>0.094 ± 0.002</td><td>4.70</td><td>53 689</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2006-01-23</td><td>98 483</td><td>2.461 ± 0.003</td><td>3.81</td><td rowspan="2">700007020</td><td>734 189</td></tr><tr><td>HXD</td><td>76 800</td><td>0.103 ± 0.003</td><td>5.06</td><td>36 695</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2006-01-27</td><td>96 691</td><td>2.708 ± 0.003</td><td>4.16</td><td rowspan="2">700007030</td><td>792 389</td></tr><tr><td>HXD</td><td>83 660</td><td>0.104 ± 0.002</td><td>4.98</td><td>40 408</td></tr><tr><td rowspan="2">Suzaku</td><td>BAT</td><td>–</td><td>–</td><td>(6.8 ± 0.3) × 10<sup>-4</sup></td><td>3.86</td><td>–</td><td>–</td></tr><tr><td>XIS</td><td rowspan="2">2007-09-17</td><td>98 748</td><td>2.863 ± 0.004</td><td>6.48</td><td rowspan="2">702112010</td><td>568 883</td></tr><tr><td>HXD</td><td>82 900</td><td>0.196 ± 0.003</td><td>10.44</td><td>43 023</td></tr><tr><td rowspan="2">Suzaku</td><td>BAT</td><td>–</td><td>–</td><td>(8.8 ± 0.2) × 10<sup>-4</sup></td><td>6.27</td><td>–</td><td>2082</td></tr><tr><td>XIS</td><td rowspan="2">2009-05-07</td><td>136 924</td><td>2.089 ± 0.003</td><td>4.23</td><td rowspan="2">704055010</td><td>576 608</td></tr><tr><td>HXD</td><td>103 800</td><td>0.101 ± 0.002</td><td>5.47</td><td>40 562</td></tr><tr><td rowspan="2">Suzaku</td><td>BAT</td><td>–</td><td>–</td><td>(9.1 ± 0.2) × 10<sup>-4</sup></td><td>6.02</td><td>–</td><td>–</td></tr><tr><td>XIS</td><td rowspan="2">2007-04-03</td><td>83 704</td><td>0.768 ± 0.002</td><td>1.47</td><td rowspan="2">702044010</td><td>130 639</td></tr><tr><td>HXD</td><td>76 920</td><td>0.027 ± 0.002</td><td>1.79</td><td>19 777</td></tr><tr><td rowspan="2">Suzaku</td><td>BAT</td><td>–</td><td>–</td><td>(4.1 ± 0.2) × 10<sup>-4</sup></td><td>2.87</td><td>–</td><td>–</td></tr><tr><td>XIS</td><td rowspan="2">2007-11-02</td><td>90 871</td><td>1.220 ± 0.003</td><td>2.13</td><td rowspan="2">702124010</td><td>224 098</td></tr><tr><td>HXD</td><td>80 370</td><td>0.053 ± 0.002</td><td>2.99</td><td>26 958</td></tr><tr><td rowspan="2">Suzaku</td><td>BAT</td><td>–</td><td>–</td><td>(5.4 ± 0.3) × 10<sup>-4</sup></td><td>3.95</td><td>–</td><td>2128</td></tr><tr><td>XIS</td><td rowspan="2">2010-05-22</td><td>100 961</td><td>0.501 ± 0.002</td><td>0.93</td><td rowspan="2">705062010</td><td>103 464</td></tr><tr><td>HXD</td><td>85 280</td><td>0.019 ± 0.001</td><td>1.94</td><td>13 647</td></tr><tr><td rowspan="2">Suzaku</td><td>BAT</td><td>–</td><td>–</td><td>(1.4 ± 0.2) × 10<sup>-4</sup></td><td>1.05</td><td>–</td><td>–</td></tr><tr><td>XIS</td><td rowspan="2">2009-05-14</td><td>160 351</td><td>0.263 ± 0.001</td><td>0.49</td><td rowspan="2">704031010</td><td>88 122</td></tr><tr><td>HXD</td><td>139 800</td><td>0.024 ± 0.001</td><td>2.42</td><td>29 520</td></tr><tr><td rowspan="2">Suzaku</td><td>BAT</td><td>–</td><td>–</td><td>(5.2 ± 0.3) × 10<sup>-4</sup></td><td>3.93</td><td>–</td><td>2617</td></tr><tr><td>XIS</td><td rowspan="2">2006-08-21</td><td>151 296</td><td>1.324 ± 0.002</td><td>1.49</td><td rowspan="2">701031010</td><td>606 927</td></tr><tr><td>HXD</td><td>131 744</td><td>0.012 ± 0.001</td><td>1.31</td><td>22 385</td></tr><tr><td rowspan="2">Suzaku</td><td>BAT</td><td>–</td><td>–</td><td>(2.5 ± 0.3) × 10<sup>-4</sup></td><td>1.81</td><td>–</td><td>830</td></tr><tr><td>XIS</td><td rowspan="2">2007-02-06</td><td>107 507</td><td>0.329 ± 0.001</td><td>0.52</td><td rowspan="2">701082010</td><td>73 004</td></tr><tr><td>HXD</td><td>96 130</td><td>0.007 ± 0.001</td><td>0.98</td><td>13 136</td></tr><tr><td rowspan="2">Suzaku</td><td>BAT</td><td>–</td><td>–</td><td>(1.2 ± 0.1) × 10<sup>-4</sup></td><td>0.92</td><td>–</td><td>–</td></tr><tr><td>XIS</td><td rowspan="2">2006-04-25</td><td>24 576</td><td>2.984 ± 0.006</td><td>4.68</td><td rowspan="2">701093010</td><td>221 506</td></tr><tr><td>HXD</td><td>14 510</td><td>0.143 ± 0.006</td><td>7.50</td><td>6647</td></tr></tbody></table>
<table><caption>Table B1 – continued</caption><thead><tr><th>Object</th><th>Mission</th><th>Instrument</th><th>Date</th><th>Exposure (s)</th><th>Count rate</th><th>Flux<sup>a</sup></th><th>ObsID</th><th>No. counts</th></tr></thead><tbody><tr><td rowspan="6">Mrk 509</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2006-10-14</td><td>25 930</td><td>3.802 ± 0.007</td><td>4.98</td><td rowspan="2">701093020</td><td>297 900</td></tr><tr><td>HXD</td><td>21 880</td><td>0.128 ± 0.005</td><td>7.89</td><td>9680</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2006-11-15</td><td>24 447</td><td>3.792 ± 0.009</td><td>4.74</td><td rowspan="2">701093030</td><td>186 702</td></tr><tr><td>HXD</td><td>17 340</td><td>0.118 ± 0.005</td><td>7.57</td><td>7260</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2006-11-27</td><td>33 094</td><td>3.278 ± 0.007</td><td>4.73</td><td rowspan="2">701093040</td><td>218 248</td></tr><tr><td>HXD</td><td>27 560</td><td>0.110 ± 0.004</td><td>7.19</td><td>11 925</td></tr><tr><td rowspan="6">Mrk 766</td><td rowspan="2">Swift</td><td>BAT</td><td rowspan="2">-</td><td>-</td><td>(8.4 ± 0.2) × 10<sup>-4</sup></td><td>6.53</td><td rowspan="2">701035010</td><td>183 736</td></tr><tr><td></td><td></td><td></td><td></td><td>26 879</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2006-11-16</td><td>97 869</td><td>0.927 ± 0.002</td><td>1.32</td><td rowspan="2">701035010</td><td>82 749</td></tr><tr><td>HXD</td><td>90 500</td><td>0.025 ± 0.002</td><td>1.48</td><td>8974</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007-11-17</td><td>59 364</td><td>0.685 ± 0.002</td><td>1.36</td><td rowspan="2">701035020</td><td>82 749</td></tr><tr><td>HXD</td><td>47 660</td><td>0.024 ± 0.002</td><td>1.67</td><td>8974</td></tr><tr><td rowspan="6">Mrk 841</td><td rowspan="2">Swift</td><td>BAT</td><td rowspan="2">-</td><td>-</td><td>(2.5 ± 0.2) × 10<sup>-4</sup></td><td>1.66</td><td rowspan="2">701084010</td><td>86 781</td></tr><tr><td></td><td></td><td></td><td></td><td>11 274</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007-01-22</td><td>51 753</td><td>0.819 ± 0.003</td><td>1.40</td><td rowspan="2">701084010</td><td>11 274</td></tr><tr><td>HXD</td><td>40 710</td><td>0.039 ± 0.003</td><td>2.42</td><td>86 626</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2007-07-23</td><td>50 925</td><td>0.830 ± 0.003</td><td>1.44</td><td rowspan="2">701084020</td><td>13 282</td></tr><tr><td>HXD</td><td>44 370</td><td>0.054 ± 0.003</td><td>2.82</td><td>13 282</td></tr><tr><td rowspan="6">NGC 1365</td><td rowspan="2">Swift</td><td>BAT</td><td rowspan="2">-</td><td>-</td><td>(3.2 ± 0.2) × 10<sup>-4</sup></td><td>2.29</td><td rowspan="2">702047010</td><td>107 383</td></tr><tr><td></td><td></td><td></td><td></td><td>55 436</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2008-01-21</td><td>160 506</td><td>0.326 ± 0.001</td><td>1.28</td><td rowspan="2">702047010</td><td>55 436</td></tr><tr><td>HXD</td><td>136 600</td><td>0.084 ± 0.002</td><td>4.72</td><td>51 909</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2010-06-27</td><td>151 613</td><td>0.159 ± 0.001</td><td>0.61</td><td rowspan="2">705031010</td><td>38 083</td></tr><tr><td>HXD</td><td>114 300</td><td>0.070 ± 0.002</td><td>4.33</td><td>77 717</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2010-07-15</td><td>302 175</td><td>0.116 ± 0.001</td><td>0.39</td><td rowspan="2">705031020</td><td>84 887</td></tr><tr><td>HXD</td><td>231 500</td><td>0.060 ± 0.001</td><td>3.49</td><td>84 887</td></tr><tr><td rowspan="6">NGC 2992</td><td rowspan="2">Swift</td><td>BAT</td><td rowspan="2">-</td><td>-</td><td>(5.2 ± 0.1) × 10<sup>-4</sup></td><td>5.11</td><td rowspan="2">700005010</td><td>43 167</td></tr><tr><td></td><td></td><td></td><td></td><td>7137</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2005-11-06</td><td>37 503</td><td>0.372 ± 0.002</td><td>1.04</td><td rowspan="2">700005010</td><td>56 041</td></tr><tr><td>HXD</td><td>29 900</td><td>0.020 ± 0.003</td><td>1.71</td><td>10 370</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2005-11-19</td><td>37 494</td><td>0.486 ± 0.002</td><td>1.37</td><td rowspan="2">700005020</td><td>59 084</td></tr><tr><td>HXD</td><td>31 890</td><td>0.042 ± 0.003</td><td>2.23</td><td>15 070</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2005-12-13</td><td>46 836</td><td>0.408 ± 0.002</td><td>1.15</td><td rowspan="2">700005030</td><td>15 070</td></tr><tr><td>HXD</td><td>41 470</td><td>0.047 ± 0.003</td><td>2.44</td><td>15 070</td></tr><tr><td rowspan="6">NGC 3147</td><td rowspan="2">Swift</td><td>BAT</td><td rowspan="2">-</td><td>-</td><td>(2.6 ± 0.2) × 10<sup>-4</sup></td><td>1.84</td><td rowspan="2">705054010</td><td>31 054</td></tr><tr><td></td><td></td><td></td><td></td><td>21 785</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2008-10-28</td><td>58 917</td><td>1.475 ± 0.004</td><td>3.91</td><td rowspan="2">703022010</td><td>175 651</td></tr><tr><td>HXD</td><td>48 070</td><td>0.145 ± 0.003</td><td>5.58</td><td>21 550</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2008-11-04</td><td>53 700</td><td>0.496 ± 0.002</td><td>1.85</td><td rowspan="2">703022020</td><td>54 717</td></tr><tr><td>HXD</td><td>46 740</td><td>0.123 ± 0.003</td><td>7.26</td><td>18 735</td></tr><tr><td rowspan="6">NGC 3227</td><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2008-11-12</td><td>56 572</td><td>0.707 ± 0.003</td><td>2.58</td><td rowspan="2">703022030</td><td>81 449</td></tr><tr><td>HXD</td><td>46 680</td><td>0.117 ± 0.003</td><td>6.78</td><td>18 919</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2008-11-20</td><td>64 568</td><td>0.278 ± 0.002</td><td>1.01</td><td rowspan="2">703022040</td><td>37 518</td></tr><tr><td>HXD</td><td>43 430</td><td>0.083 ± 0.003</td><td>4.82</td><td>17 263</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2008-11-27</td><td>79 430</td><td>0.568 ± 0.002</td><td>2.16</td><td rowspan="2">703022050</td><td>92 162</td></tr><tr><td>HXD</td><td>37 420</td><td>0.104 ± 0.003</td><td>6.26</td><td>14 795</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2008-12-02</td><td>51 411</td><td>0.413 ± 0.002</td><td>1.61</td><td rowspan="2">703022060</td><td>43 570</td></tr><tr><td>HXD</td><td>36 910</td><td>0.082 ± 0.003</td><td>5.70</td><td>13 177</td></tr><tr><td rowspan="6">NGC 3516</td><td rowspan="2">Swift</td><td>BAT</td><td rowspan="2">-</td><td>-</td><td>(10.3 ± 0.2) × 10<sup>-4</sup></td><td>7.68</td><td rowspan="2">100031010</td><td>289 936</td></tr><tr><td></td><td></td><td></td><td></td><td>49 782</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2009-10-28</td><td>251 356</td><td>0.456 ± 0.001</td><td>1.35</td><td rowspan="2">704062010</td><td>235 894</td></tr><tr><td>HXD</td><td>178 200</td><td>0.059 ± 0.001</td><td>3.32</td><td>58 222</td></tr><tr><td rowspan="6">NGC 3783</td><td rowspan="2">Swift</td><td>BAT</td><td rowspan="2">-</td><td>-</td><td>(10.5 ± 0.2) × 10<sup>-4</sup></td><td>7.76</td><td rowspan="2">701033010</td><td>416 485</td></tr><tr><td></td><td></td><td></td><td></td><td>33 592</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2006-06-24</td><td>75 719</td><td>2.066 ± 0.003</td><td>4.59</td><td rowspan="2">701033010</td><td>805 999</td></tr><tr><td>HXD</td><td>63 930</td><td>0.167 ± 0.003</td><td>9.26</td><td>87 319</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2009-07-10</td><td>209 503</td><td>1.942 ± 0.002</td><td>5.92</td><td rowspan="2">704063010</td><td>1036 060</td></tr><tr><td>HXD</td><td>162 000</td><td>0.235 ± 0.002</td><td>12.04</td><td>75 619</td></tr><tr><td rowspan="6">NGC 4051</td><td rowspan="2">Swift</td><td>BAT</td><td rowspan="2">-</td><td>-</td><td>(16.6 ± 0.2) × 10<sup>-4</sup></td><td>11.54</td><td rowspan="2">700004010</td><td>149 284</td></tr><tr><td></td><td></td><td></td><td></td><td>29 700</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2005-11-10</td><td>119 578</td><td>0.406 ± 0.001</td><td>0.87</td><td rowspan="2">700004010</td><td>1036 060</td></tr><tr><td>HXD</td><td>112 600</td><td>0.037 ± 0.002</td><td>1.63</td><td>29 700</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2008-11-06</td><td>274 350</td><td>1.858 ± 0.002</td><td>2.46</td><td rowspan="2">703023020</td><td>75 619</td></tr><tr><td>HXD</td><td>204 500</td><td>0.062 ± 0.001</td><td>3.05</td><td>202 942</td></tr><tr><td rowspan="2">Suzaku</td><td>XIS</td><td rowspan="2">2008-11-23</td><td>78 385</td><td>1.276 ± 0.003</td><td>1.79</td><td rowspan="2">703023010</td><td>21 296</td></tr><tr><td>HXD</td><td>58 530</td><td>0.048 ± 0.002</td><td>2.54</td><td>21 296</td></tr><tr><td rowspan="2">Swift</td><td>BAT</td><td rowspan="2">-</td><td>-</td><td>(4.0 ± 0.2) × 10<sup>-4</sup></td><td>2.80</td><td rowspan="2">703023010</td><td>21 296</td></tr><tr><td></td><td></td><td></td><td></td><td></td></tr></tbody></table>
<table><caption>Table B1 – continued</caption><thead><tr><th>Object</th><th>Mission</th><th>Instrument</th><th>Date</th><th>Exposure (s)</th><th>Count rate</th><th>Flux<sup>a</sup></th><th>ObsID</th><th>No. counts</th></tr></thead><tbody><tr><td rowspan="3">NGC 4151</td><td>Suzaku</td><td>XIS</td><td>2006-12-18</td><td>124 980</td><td>1.036 ± 0.002</td><td>4.35</td><td rowspan="3">701034010</td><td>262 831</td></tr><tr><td></td><td>HXD</td><td></td><td>123 500</td><td>0.293 ± 0.002</td><td>15.90</td><td>78 564</td></tr><tr><td>Swift</td><td>BAT</td><td>–</td><td>–</td><td>(43.6 ± 0.2) × 10<sup>-4</sup></td><td>32.50</td><td></td></tr><tr><td rowspan="3">NGC 4593</td><td>Suzaku</td><td>XIS</td><td>2007-12-15</td><td>118 842</td><td>0.524 ± 0.002</td><td>1.04</td><td rowspan="3">702040010</td><td>127 503</td></tr><tr><td></td><td>HXD</td><td></td><td>101 600</td><td>0.033 ± 0.002</td><td>2.15</td><td>30 049</td></tr><tr><td>Swift</td><td>BAT</td><td>–</td><td>–</td><td>(7.3 ± 0.2) × 10<sup>-4</sup></td><td>5.74</td><td></td></tr><tr><td rowspan="6">NGC 5506</td><td>Suzaku</td><td>XIS</td><td>2006-08-08</td><td>47 753</td><td>3.064 ± 0.005</td><td>10.05</td><td rowspan="6">701030010</td><td>441 844</td></tr><tr><td></td><td>HXD</td><td></td><td>38 550</td><td>0.324 ± 0.004</td><td>17.30</td><td>25 416</td></tr><tr><td>Suzaku</td><td>XIS</td><td>2006-08-11</td><td>53 296</td><td>3.230 ± 0.005</td><td>10.58</td><td>519 889</td></tr><tr><td></td><td>HXD</td><td></td><td>44 830</td><td>0.343 ± 0.004</td><td>18.40</td><td>30 625</td></tr><tr><td>Suzaku</td><td>XIS</td><td>2007-01-31</td><td>57 406</td><td>2.854 ± 0.005</td><td>9.90</td><td>330 141</td></tr><tr><td></td><td>HXD</td><td></td><td>44 670</td><td>0.321 ± 0.004</td><td>17.11</td><td>29 399</td></tr><tr><td>Swift</td><td>BAT</td><td>–</td><td>–</td><td>(23.2 ± 0.2) × 10<sup>-4</sup></td><td>15.95</td><td></td></tr><tr><td rowspan="10">NGC 5548</td><td>Suzaku</td><td>XIS</td><td>2007-06-18</td><td>31 119</td><td>0.369 ± 0.003</td><td>0.81</td><td rowspan="10">702042010</td><td>23 857</td></tr><tr><td></td><td>HXD</td><td></td><td>25 590</td><td>0.046 ± 0.004</td><td>2.70</td><td>9397</td></tr><tr><td>Suzaku</td><td>XIS</td><td>2007-06-24</td><td>35 915</td><td>0.650 ± 0.003</td><td>1.34</td><td>47 786</td></tr><tr><td></td><td>HXD</td><td></td><td>31 210</td><td>0.050 ± 0.003</td><td>3.12</td><td>9880</td></tr><tr><td>Suzaku</td><td>XIS</td><td>2007-07-08</td><td>30 700</td><td>1.349 ± 0.005</td><td>2.54</td><td>83 863</td></tr><tr><td></td><td>HXD</td><td></td><td>26 960</td><td>0.064 ± 0.004</td><td>4.34</td><td>9824</td></tr><tr><td>Suzaku</td><td>XIS</td><td>2007-07-15</td><td>30 020</td><td>0.834 ± 0.004</td><td>1.74</td><td>51 085</td></tr><tr><td></td><td>HXD</td><td></td><td>24 470</td><td>0.062 ± 0.004</td><td>4.16</td><td>7612</td></tr><tr><td>Suzaku</td><td>XIS</td><td>2007-07-22</td><td>28 918</td><td>1.656 ± 0.005</td><td>3.28</td><td>96 936</td></tr><tr><td></td><td>HXD</td><td></td><td>23 060</td><td>0.095 ± 0.004</td><td>0.22</td><td>8336</td></tr><tr><td>Suzaku</td><td>XIS</td><td>2007-07-29</td><td>31 810</td><td>1.075 ± 0.004</td><td>2.19</td><td>69 507</td></tr><tr><td></td><td>HXD</td><td></td><td>27 610</td><td>0.075 ± 0.004</td><td>4.71</td><td>9377</td></tr><tr><td>Suzaku</td><td>XIS</td><td>2007-08-05</td><td>38 776</td><td>0.558 ± 0.003</td><td>1.19</td><td>44 486</td></tr><tr><td></td><td>HXD</td><td></td><td>30 380</td><td>0.054 ± 0.003</td><td>3.41</td><td>9958</td></tr><tr><td>Swift</td><td>BAT</td><td>–</td><td>–</td><td>(6.1 ± 0.2) × 10<sup>-4</sup></td><td>4.56</td><td></td></tr><tr><td rowspan="3">NGC 7213</td><td>Suzaku</td><td>XIS</td><td>2006-10-22</td><td>90 736</td><td>1.528 ± 0.002</td><td>2.41</td><td rowspan="3">701029010</td><td>419 604</td></tr><tr><td></td><td>HXD</td><td></td><td>84 290</td><td>0.064 ± 0.002</td><td>3.48</td><td>33 910</td></tr><tr><td>Swift</td><td>BAT</td><td>–</td><td>–</td><td>(3.6 ± 0.2) × 10<sup>-4</sup></td><td>5.13</td><td></td></tr><tr><td rowspan="3">NGC 7314</td><td>Suzaku</td><td>XIS</td><td>2007-04-25</td><td>109 020</td><td>0.296 ± 0.001</td><td>0.88</td><td rowspan="3">702015010</td><td>67 434</td></tr><tr><td></td><td>HXD</td><td></td><td>85 780</td><td>0.026 ± 0.002</td><td>1.43</td><td>25 675</td></tr><tr><td>Swift</td><td>BAT</td><td>–</td><td>–</td><td>(4.6 ± 0.2) × 10<sup>-4</sup></td><td>3.62</td><td></td></tr><tr><td rowspan="3">NGC 7469</td><td>Suzaku</td><td>XIS</td><td>2008-06-24</td><td>112 113</td><td>1.091 ± 0.002</td><td>2.10</td><td rowspan="3">703028010</td><td>248 180</td></tr><tr><td></td><td>HXD</td><td></td><td>85 315</td><td>0.068 ± 0.002</td><td>3.22</td><td>29 831</td></tr><tr><td>Swift</td><td>BAT</td><td>–</td><td>3286 000</td><td>(6.6 ± 0.3) × 10<sup>-4</sup></td><td>4.87</td><td>2179</td></tr><tr><td rowspan="2">PDS 456</td><td>Suzaku</td><td>XIS</td><td>2007-02-24</td><td>190 600</td><td>0.237 ± 0.001</td><td>0.35</td><td rowspan="2">701056010</td><td>92 499</td></tr><tr><td></td><td>HXD</td><td></td><td>64 150</td><td>0.012 ± 0.003</td><td>0.25</td><td>20 372</td></tr><tr><td rowspan="2">PG 1211+143</td><td>Suzaku</td><td>XIS</td><td>2005-11-24</td><td>96 324</td><td>0.268 ± 0.001</td><td>0.39</td><td rowspan="2">700009010</td><td>81 584</td></tr><tr><td></td><td>HXD</td><td></td><td>78 800</td><td>0.004 ± 0.002</td><td>0.50</td><td>29 181</td></tr><tr><td rowspan="2">RBS 1124</td><td>Suzaku</td><td>XIS</td><td>2007-04-14</td><td>86 228</td><td>0.260 ± 0.001</td><td>0.49</td><td rowspan="2">702114010</td><td>46 699</td></tr><tr><td></td><td>HXD</td><td></td><td>82 970</td><td>0.016 ± 0.001</td><td>0.91</td><td>14 206</td></tr><tr><td rowspan="3">SWIFT J2127.4+5654</td><td>Suzaku</td><td>XIS</td><td>2007-12-09</td><td>91 730</td><td>1.373 ± 0.004</td><td>3.35</td><td rowspan="3">702122010</td><td>127 435</td></tr><tr><td></td><td>HXD</td><td></td><td>83 321</td><td>0.074 ± 0.002</td><td>3.33</td><td>27 970</td></tr><tr><td>Swift</td><td>BAT</td><td>–</td><td>–</td><td>(4.3 ± 0.3) × 10<sup>-4</sup></td><td>3.62</td><td>1689</td></tr><tr><td rowspan="2">TON S180</td><td>Suzaku</td><td>XIS</td><td>2006-12-09</td><td>120 661</td><td>0.701 ± 0.002</td><td>0.56</td><td rowspan="2">701021010</td><td>172 889</td></tr><tr><td></td><td>HXD</td><td></td><td>102 400</td><td>0.012 ± 0.002</td><td>0.77</td><td>27 241</td></tr></tbody></table>

<footnote><sup>a</sup>The observed 2–10 keV flux for XIS, 15–50 keV flux for HXD and 20–100 keV flux for BAT, in units $10^{-11}$ erg cm$^{-2}$ s$^{-1}$, from the baseline model.</footnote>