A&A 493, 445-451 (2009)
DOI: 10.1051/0004-6361:200809665
A. Del Moro1 - M. G. Watson1 - S. Mateos1 - M. Akiyama2 - Y. Hashimoto3 - N. Tamura4 - K. Ohta5 - F. J. Carrera6 - G. Stewart1
1 - XROA-University of Leicester, University Road, Leicester LE1 7RH, UK
2 - Astronomical Institute, Tohoku University, Sendai 980-8578, Japan
3 - South African Astronomical Observatory, Observatory Road, Cape Town 7539, South Africa
4 - Subaru Telescope, National Astronomical Observatory of Japan, Hilo, HI 96720, Japan
5 - Department of Astronomy, Kyoto University, Kyoto 606-8502, Japan
6 - Instituto de Física de Cantabria (CSIC-UC), Avenida de los Castros, 39005 Santander, Spain
Receievd 27 February 2008 / Accepted 23 September 2008
Abstract
Aims. We aim to understand the multi-wavelength properties of 2XMM J123204+215255, the source with the most extreme X-ray-to-optical flux ratio amongst a sample of bright X-ray selected EXOs drawn from a cross-correlation of the 2XMMp catalogue with the SDSS-DR5 catalogue.
Methods. We use 2XMMp X-ray data, SDSS-DR5, NOT and UKIRT optical/NIR photometric data and Subaru MOIRCS IR spectroscopy to study the properties of 2XMM J123204+215255. We created a model SED including an obscured QSO and the host galaxy component to constrain the optical/IR extinction and the relative contribution of the AGN and the galaxy to the total emission.
Results. 2XMM J123204+215255 is a bright X-ray source with
erg cm-2 s-1 (2-10 keV energy band) which has no detection down to a magnitude i'>25.2. NIR imaging reveals a faint K-band counterpart and NIR spectroscopy shows a single broad (
km s-1) emission line, which is almost certainly H
at z=1.87. The X-ray spectrum shows evidence of significant absorption (
), typical of type 2 AGN, but the broad H
emission suggests a type 1 AGN classification. The very red optical/NIR colours (i'-K>5.3) strongly suggest significant reddening however. We find that simple modelling can successfully reproduce the NIR continuum and strongly constrain the intrinsic nuclear optical/IR extinction to
,
which turns out to be much smaller than the expected from the X-ray absorption (assuming Galactic gas-to-dust ratio).
Key words: galaxies: active - galaxies: quasars: general - X-rays: galaxies - infrared: galaxies
Over the past few years, extensive studies have been carried out to determine the complete census of the active
galactic nuclei (AGN) population, in particular the bright, obscured objects (optically type 2 QSOs), invoked by the
synthesis models of the X-ray background (XRB, Gilli et al. 2007; Comastri 2001; Setti & Woltjer 1989; Comastri et al. 1995; Gilli et al. 2001).
The deepest surveys carried out to date by Chandra and XMM-Newton have resolved >
(Mushotzky et al. 2000; Alexander et al. 2003; Hasinger et al. 2001) of the XRB spectrum at energies below 5 keV, however a large number of the obscured AGN
are still missing. For these reasons, many studies have been addressed to reveal this elusive class of objects, primarily
focused on the X-ray band, but also involving multi-wavelength studies (Zakamska et al. 2003,2004; Martínez-Sansigre et al. 2006).
In previous studies, the X-ray-to-optical-flux ratio (
), defined here as the ratio between the X-ray flux (usually in the
2-10 keV energy band) and R-band flux, has been commonly used to provide a first classification of the X-ray population
(Maccacaro et al. 1988): normal galaxies have typically
0.1 (e.g. Lehmann et al. 2001; Giacconi et al. 2001) while the
dominant X-ray selected AGN population has 0.1<
<10 (e.g. Fiore et al. 2003; Akiyama et al. 2000; Alexander et al. 2001); obscured AGN
typically have
10 or above (e.g. Mignoli et al. 2004).
Recently, a new interesting class of objects with extreme values of the X-ray-to-optical flux ratio (
> 10) has
been found from deep X-ray surveys; these objects, called Extreme X-ray-to-Optical ratio sources
(EXOs, Koekemoer et al. 2004), are usually detected in X-rays and in near-IR, but completely undetected in the optical
bands. Although a few turn out to be BL Lac objects, high-redshift clusters of galaxies or rare Galactic objects (e.g.
X-ray binaries, cataclysmic variables, isolated neutron stars or ultraluminous X-ray sources), the majority are
almost certainly type 2 AGN (Fiore et al. 2003), where the nucleus is heavily obscured by dust in the UV/optical/IR
whilst the X-ray flux, although strongly absorbed at low energies (below
2 keV), is much less affected by
absorption above
2 keV.
As expected in this scenario, a significant fraction of the EXO population shows the extremely red colours of EROs
(extremely red objects, typical ,
Elston et al. 1988; see Fiore et al. 2003; Mignoli et al. 2004). EXOs with
optical-NIR colours of EROs are thus amongst the best candidates to be highly absorbed, highly obscured AGN, i.e. type 2 AGN.
However, almost by definition, sources with such extreme
have faint optical magnitudes and this is even more true
for the faint X-ray sources found in the deep, pencil-beam surveys (Koekemoer et al. 2004; Civano et al. 2005). At such faint X-ray
fluxes (
=
10-15-10-16 erg cm-2 s-1), sources with
> 10
have R magnitudes
25.5-28, so the optical follow-up
observations are very difficult or impossible. Studies performed at higher X-ray fluxes (
=
10-14-10-13 erg cm-2 s-1,
e.g. Fiore et al. 2003; Mignoli et al. 2004; Severgnini et al. 2006), for which optical data are available, have classified more than a
half of their EXO sources as type 2 QSOs.
In this paper, we report the results obtained from the multi-wavelength analysis of 2XMM J123204+215255, the most
extreme source amongst a sample of 130 bright (
10-13 erg cm-2 s-1) X-ray selected EXOs (Del Moro et al., in prep.) from the 2XMMp catalogue (the pre-release of the Second XMM-Newton Serendipitous Source Catalogue, Watson et al. 2008).
The whole sample is described in Sect. 2.1. The X-ray and optical/NIR properties of 2XMM J123204+215255 are discussed in Sects. 2.2 and 2.3, respectively; a detailed description of the NIR spectrum is presented in
Sect. 2.4. An SED model analysis and results are discussed in
Sect. 3, followed by the conclusions (Sect. 4). Throughout the
paper we assume a cosmological model with
,
and
(Spergel et al. 2003).
The object we present in this paper is part of a sample selected from a cross-correlation between the 2XMMp and the Sloan Digital Sky Survey, Data Release 5
(SDSS-DR5, Adelman-McCarthy et al. 2007) catalogues, which yields about 20 000 secure matches. SDSS optical counterparts have been
selected on the basis of positional matching, using an adaptation of the likelihood ratio method (e.g. Sutherland & Saunders 1992)
to optimise the choice of correct counterpart and minimise the contamination by chance matches. Full details of our approach
will appear in Del Moro et al., in preparation.
Our sample consists of relatively bright X-ray sources with
10-13 erg cm-2 s-1 (0.2-12 keV energy band) and extreme
X-ray-to-optical flux ratio (
> 10, in the 2-10 keV band).
Each XMM and SDSS image of the sample objects has been
carefully checked by eye in order to reject all the problematic cases: spurious X-ray detections, sources close to the edge of
the XMM-Newton field of view, extended X-ray sources
,
optical counterparts in big nearby galaxies (HII region emissions). Because we are selecting extreme X-ray-to-optical flux
ratio objects, the counterparts of our sources are typically faint in the optical, at our sensitivity limits,
making it difficult in some cases to differentiate between the possibility that the true match is fainter than the SDSS limit or
that the correct counterpart is a faint object with low likelihood ratio (and hence with a higher probability to be a
chance match). The effects of this ambiguity are that the
values, in these cases, will be underestimated (i.e. if
the counterpart is fainter than the SDSS limit). In this sense our sample is robust.
The sample resulting from these selection processes consists of 130 sources for which 30% (including 2XMM J123204+215255) have no
optical counterpart in the SDSS imaging data within 7
from the X-ray position (see Sect. 2.2), down to a
magnitude limit of r'=22.5.
The source 2XMM J123204+215255 is the most extreme X-ray-to-optical flux ratio object amongst our EXO sample. It is a bright X-ray
source with
=
erg cm-2 s-1 (in the 2-10 keV energy band). On the basis of the lack of an SDSS
counterpart it has
> 278, already one of the highest ratios recorded, whilst as we show below, new data demonstrate the
ratio to be
> 3300, making it the highest known X-ray-to-optical flux ratio source outside the Galaxy. The source
has been detected in an XMM-Newton observation with target ``NGP Rift 3'' which was made in July 2001 with an exposure
time of
15 ks with pn and
20 ks with MOS1 and MOS2.
The statistical position error for 2XMM J123204+215255 is 0.3
.
Taking into account the expected systematic error component for the
2XMMp catalogue of 0.35
,
determined from a comparison of catalogue positions with the SDSS-DR5 Quasar Catalog
(see Watson et al. 2008), we expect the counterpart to lie within
1.4
(99% confidence). The
comparison with the SDSS Quasar Catalog shows that there are a very small number of outliers at larger separations in excess
of what is expected statistically (presumably indicating a larger systematic error component in these rare cases), but in no
case the separation is >7 arcsec. We adopt this value as the most conservative upper limit on the possible separation of
the true counterpart.
To study the X-ray spectrum of 2XMM J123204+215255, the data have been processed using the standard SAS v.7.1.0 tasks (XMM-Newton Science
Analysis System, Gabriel et al. 2004). We extracted the spectrum of the source using an elliptical region to reproduce the
shape of the Point Spread Function (PSF) of the XMM Telescopes at the source position. The corresponding background spectrum
has been extracted using an annular region with radii 30
and 90
,
centred on the source position, removing any
other detected nearby sources. The data have been then filtered for high background intervals. The total EPIC number of
counts in the 0.2-12 keV energy band after the filtering is 2234. The spectral analysis has been performed with XSPEC v.11.3.2 (Arnaud 1996), grouping the number of counts to a minimum of 10 counts per bin, in order to use the
statistic. We find an acceptable fit to a simple model composed of a power-law plus Galactic and intrinsic absorptions;
fixing
,
the best fit parameters are photon index
and hydrogen
column density
(assuming z=0), with
.
Repeating the X-ray spectral analysis for z=1.87, anticipating the result presented below (Sect. 2.4), we obtained a best
fit to the data with a photon index
and a column density
(Fig. 1). We note the presence of marginally significant structure in the spectrum residuals at energy
1.5-3 keV which might be related to red-shifted line or edge features. The reality of these features clearly require
confirmation at higher signal-to-noise.
We obtained deeper optical imaging of the field on 2007 February 9 on the 2.5 m NOT (Nordic Optical Telescope).
Four separate i'-band images were taken with the NOT ALFOSC camera with integration times of 1800 s each.
Conditions were photometric with 1 arcsec seeing, but unfortunately the images are affected by bad fringing. As
there were no sky flats available to correct properly for the fringing, an empirical approach was adopted in which a
smoothed version of each image (with bright objects removed) is used to estimate the effective sky background plus
fringing effects. The resultant background-subtracted images were then stacked to make the final image (Fig. 2). This technique does not fully remove the fringing effects, but reduces them to a modest level,
significantly improving the sensitivity for faint objects.
We find no detection of any counterpart within 7 arcsec of the position of 2XMM J123204+215255 with an estimated 5
limit i'>25.2
mag, based on the amplitude of the residual background fluctuations. The photometric calibration was established by comparing
the count rates of a sample of objects detected in the NOT image with the SDSS-DR5 photometric catalogue.
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Figure 1:
EPIC pn, MOS1 and MOS2 X-ray spectrum of 2XMM J123204+215255 ( top panel): the model is represented by the black
lines; residuals are also shown ( lower panel).
The data are well represented by an absorbed power-law with a photon index
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As the object is likely to be heavily obscured in the optical, the obvious next step is IR observations, where the effective
dust obscuration will be lower. Follow-up J-band and K-band observations of 2XMM J123204+215255 have been obtained with the UK
Infrared Telescope-Wide Field Infrared Camera (UKIRT-WFCAM) the
of February 2007 with an exposure time of 1200 s
in the J-band and
s in the K-band. The IR images
(Fig. 2) show an apparently stellar
counterpart in the K-band with a magnitude
(Vega,
magnitude system,
Oke & Gunn 1983; see Hewett et al. 2006) and a very marginal detection in the
J-band (
,
Vega). All the
values are reported in Table 1. The IR counterpart lies
1
from the X-ray centroid, consistent with
the position errors discussed in Sect. 2.2. The IR detection allows us to place limits on the optical/IR colours of the
source: r'-K>2.6 and i'-K>5.3 (AB). As the optical emission is likely to be dominated by a high redshift galaxy, as
discussed below, it is likely that r'-i'>0, which means that the r' magnitude should be of the order of
.
If
that is true, the r'-K colour becomes greater than 5.3 (AB), corresponding to r'-K>7 in the Vega system, which is
extremely red even for EROs (Sect. 1).
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Figure 2:
Optical/IR finding charts for 2XMM J123204+215255.
From left to right: SDSS r'-band image, NOT
i'-band stacked image, UKIRT-WFCAM J and K bands. The
K-band image shows an apparently stellar counterpart
(
K=19.9, AB). The circles have a radius of 7
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Table 1: Multi-wavelength properties of 2XMM J123204+215255.
We took 6 target frames with 7 min exposure each, thus the total on-source integration time was 42 min. The
telescope was dithered after every single exposure and the target was observed at different positions along the slit
(
or
from the slit centre). After sky subtraction, carried out by subtracting
adjacent object frames from each other, flat-fielding was performed using dome-flat frames. These sky-subtracted and
flat-fielded frames were then shifted, mirrored and combined to determine the average intensity value at each pixel with a 3
clipping algorithm. Atmospheric absorption correction and flux calibration have been performed using the spectrum of
a bright star (HD 119496, spectral type of A2V). The standard star spectrum was taken at the end of the night at a similar
airmass to the target and with the same instrumental setup.
The observed spectrum (Fig. 3) reveals a red continuum emission, which is well represented by
.
Using this form and extrapolating it out to the wavelengths longer than 23 000 Å, the
K-band magnitude of this source is estimated to be
mag in the
AB system without any corrections (the emission
line is at the edge of the K-band and its effect on this estimate can be ignored). This is consistent with the UKIRT-WFCAM
photometry (
,
see Sect. 2.3 and Table 1) within the uncertainties. An estimated
10% of
the total flux from the object falls outside the slit width in the
seeing conditions of the observation. As the
slit losses are uncertain and the magnitude estimates from the spectroscopy are consistent with the UKIRT imaging, we therefore
do not apply any slit-loss corrections to the emission line fluxes estimated below, but note that they have
10-20%
systematic uncertainty.
As shown in Fig. 3, a single broad emission line
(FWHM =
km s-1) is clearly visible
on the red continuum in the observed spectrum at
Å (line centroid). The line flux is
erg cm-2 s-1 (uncorrected for absorption;
Table 2). The emission line centre and line width have been estimated by fitting
a Gaussian to the spectrum in the vicinity of the line after the continuum was subtracted, whilst the line flux was estimated
by directly integrating the continuum-subtracted line profile. The derived Equivalent Width (EW) is
Å.
All the uncertainties are estimated from the 1
errors in the Gaussian fitting process.
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Figure 3:
The Subaru MOIRCS IR spectrum of 2XMM J123204+215255 (black) showing a single broad emission line (
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Although there are no other significant emission or absorption lines visible in the spectrum, the most likely
interpretation is that the line detected is H.
We also considered other possible interpretations for this line:
For a redshift z=1.87, the intrinsic X-ray luminosity for the source is
erg s-1
(2-10 keV rest-frame) and the X-ray spectrum has a large column density (
;
Sect. 2.2). The X-ray properties of 2XMM J123204+215255 are thus those of a very luminous, heavily absorbed AGN, with
spectral parameters typical for a type 2 QSO.
In contrast the IR spectrum shows a broad H emission line and the
IR counterpart detected in the K-band has a
probable stellar morphology, characteristics of a type 1 object. To further complicate the story the predicted emission
line fluxes are much higher than those observed (see Table 2). Using the correlation between hard X-ray
luminosities and H
and [O III] luminosities from Panessa et al. (2006):
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Figure 4: Best-fit model of the NIR spectrum (magenta points); green circles: photometric measurements and upperlimits of the r', i', J and K-band magnitudes; red line: galaxy SED; blue line: absorbed QSO SED; grey dash-dotted line: unabsorbed QSO SED; black line: resulting SED (QSO + host galaxy). In the lower panel the residuals of the fitting are shown. |
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Table 2: Observed and predicted line fluxes of 2XMM J123204+215255.
In order to see whether it was possible to reconcile the X-ray, optical and near IR characteristics of this object, we carried out simple modelling of the IR spectral continuum using a composite Spectral Energy Distribution (SED) with two components: one corresponding to the host galaxy and one to a typical QSO (Fig. 4). As QSOs are typically found to be hosted by massive elliptical galaxies (Dunlop et al. 2003; McLeod & Rieke 1995; Aretxaga et al. 1998), we adopted a 5 Gyr early-type galaxy template, generated with the GRASIL code (Silva et al. 1998). To reproduce the QSO we adopted a composite spectrum of a type 1 QSO with the highest IR/optical ratio (from Polletta et al. 2007). In the model the QSO SED component has intrinsic absorption, i.e. nuclear extinction, parameterised by a rest-frame equivalent AV and represented by the Small Magellanic Cloud (SMC) extinction curve from Pei (1992), whilst both the QSO and galaxy SEDs have fixed Galactic absorption (
Our modelling cannot of course be considered as definitive, as it is limited by the restricted wavelength coverage of our data,
by the fact that we cannot be sure of the intrinsic SEDs for the galaxy and AGN components and by the assumption that just two
components will adequately represent the data. We can however examine how our results depends on the choice of the SED components in the spectral range we are investigating, by using different QSO templates (from Polletta et al. 2007) in the
fitting process. For this range of templates we find variations of
10% in the derived rest-frame equivalent AV. As
in all the models we tested the contribution of the galaxy appears to be only few percent of the total emission there is clearly
little sensitivity to the precise shape of the galaxy SED adopted.
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Figure 5:
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With the model parameters obtained from our analysis, the extinction for the QSO component in the J-band (close to H
and [O III]) corresponds to
5.3 mag and
2.4 mag in the K-band, in the vicinity of the redshifted
H
line. Correcting the observed H
flux for this extinction (AK) gives a value
erg cm-2 s-1, which is lower than the flux expected from the
correlation of Panessa et al. 2006 (see Table 2), but well within the scatter of the correlation. The much higher
extinction (
)
at the H
line is fully consistent with its non-detection.
The lack of detection of the [O III] line is not explained in the model, as this line is expected to originate in the
Narrow-Line Region (NLR) which should not be affected by the large extinction of the nuclear region. However, the
weakness or disappearance of the [O III] emission line has already been reported for high-luminosity AGN
(see Yuan & Wills 2003; Sulentic et al. 2004; Netzer et al. 2004). A possible explanation may be related to the fact that the simple scaling law:
(where
is the radius of the Narrow Line Region and
is the ionising source
luminosity, Netzer et al. 2004), which may explain the correlation between the X-ray and the [O III] luminosities at
lower values, must break down when the NLR radius becomes comparable with the size of the galaxy.
Another possible explanation may be the presence of obscuring dust outside the torus, at larger distances from the nucleus. This dust could reside in the NLR (Polletta et al. 2008) or in the host galaxy (Brand et al. 2007; Rigby et al. 2006; Martínez-Sansigre et al. 2006) and could thus absorb the emission coming from the Narrow Line Region. This interpretation is equally consistent with the observed red continuum and the extinction of the broad lines whilst also providing an explanation for the absence of any narrow lines in the IR spectrum. However, as it is not possible to constrain the location of the obscuring dust with the present data, neither interpretation can be rejected.
Finally we note that the values obtained for the optical extinction from our modelling are significantly lower than naively
expected from the measured X-ray column density. This can most easily be parameterised by a dust-to-gas ratio which is about
20-25 times lower than the standard Galactic value
(
,
e.g. Predehl & Schmitt 1995). Such low ratios have been reported in several previous studies of AGN (Akiyama et al. 2002; Willott et al. 2004; Maiolino et al. 2001b; Maccacaro et al. 1982). In this comparison, as is the case in the other papers cited, we are assuming the simplest possible
geometry where the dust and gas are co-spatial and lie in a uniform foreground screen
. One possible explanation for the high ratio is a different dust grain size distribution dominated by large grains,
whose formation is naturally expected in the high density environments, like those characterising the circumnuclear region of AGNs. This dust grain distribution makes the extinction curve flatter than the Galactic one and yields a higher
ratio (Maiolino et al. 2001a; Maiolino 2002). This would not be a valid explanation if the absorption is
on kpc-scales as discussed above.
Alternatively 2XMM J123204+215255 might be a member of a population of AGN with absorption on kpc-scales, sometimes described as ``host-obscured'' AGN (e.g. Brand et al. 2007), which may be an important ingredient in resolving the discrepancy between the predicted and observed ratios of type I and type II AGN, which exists in some models of AGN obscuration (e.g. Brand et al. 2007; Martínez-Sansigre et al. 2006).
We have shown that
selection using the large samples afforded by the 2XMM catalogue provides an effective way of
discovering extreme objects like 2XMM J123204+215255, which are a rare but important part of the obscured AGN population. Our analysis has
demonstrated that the extreme properties of this object are a natural consequence of its very high luminosity and large
obscuration. It is interesting to note that a high luminosity object of this type with only a factor of a few higher
absorption would appear as an entirely ``normal'' galaxy, in that it would have no detectable broad lines in its spectrum and
presumably no narrow lines either, given the apparent strong suppression of the NLR emission lines evident at these high
luminosities.
Acknowledgements
The data presented here include those taken using ALFOSC, which is owned by the Instituto de Astrofísica de Andalucía (IAA) and operated at the Nordic Optical Telescope under agreement between IAA and the NBIfAFG of the Astronomical Observatory of Copenhagen. The analysis in this paper are based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. The United Kingdom Infrared Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK. We gratefully acknowledge the SPARTAN support under the contract MEST-CT-2004-7512. F.J.C. acknowledges financial support by the Spanish Ministerio de Educación y Ciencia under project ESP2006-13608-C02-01. S.M. acknowledges direct support from the UK STFC research Council. We thank the referee for the constructive comments, which helped to improve the paper.