A&A 437, 805-821 (2005)
DOI: 10.1051/0004-6361:20041212
V. Mainieri1,2,3 - P. Rosati2 - P. Tozzi4 - J. Bergeron5 - R. Gilli6 - G. Hasinger1 - M. Nonino4 - I. Lehmann1 - D. M. Alexander7 - R. Idzi8 - A. M. Koekemoer8 - C. Norman9 - G. Szokoly1 - W. Zheng9
1 - Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse PF 1312,
85748 Garching bei Muenchen, Germany
2 -
European Southern Observatory,
Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany
3 -
Dip. di Fisica, Università degli Studi Roma Tre,
Via della Vasca Navale 84, 00146 Roma, Italy
4 -
INAF, Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34131 Trieste, Italy
5 -
Institut d'Astrophysique de Paris, 98bis boulevard, 75014 Paris, France
6 -
INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125, Firenze, Italy
7 -
Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK
8 -
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
9 -
Center for Astrophysical Sciences, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA
Received 2 May 2004 / Accepted 25 February 2005
Abstract
We provide important new constraints on the nature and
redshift distribution of optically faint ()
X-ray
sources in the Chandra Deep Field South Survey. We use a large
multi-wavelength data set, including the GOODS/ACS survey, the
recently released Hubble Ultra Deep Field (UDF) data, and the new
public VLT/ISAAC imaging. We show that we can derive accurate
photometric redshifts for the spectroscopically unidentified
sources thus maximizing the redshift completeness for the whole
X-ray sample. Our new redshift distribution for the X-ray source
population is in better agreement with that predicted by X-ray
background synthesis models; however, we still find an
overdensity of low redshift (z< 1) sources. The optically faint
sources are mainly X-ray absorbed AGN, as determined from direct
X-ray spectral analysis and other diagnostics.
Many of these
optically faint sources have high (>10) X-ray-to-optical flux
ratios. We also find that 71% of them are well fitted
with the SED of an early-type galaxy with
and the remaining 29% with irregular or starburst
galaxies mainly at
.
We estimate that
of
the optically faint sources are X-ray absorbed QSOs. The overall
population of X-ray absorbed QSOs contributes a
fraction of the [2-10] keV X-ray Background (XRB) whereas current
XRB synthesis models predict a
contribution.
Key words: surveys - galaxies: active - galaxies: quasars: general - cosmology: diffuse radiation - X-ray: galaxies - X-rays: general
Recent Chandra and XMM-Newton (Brandt et al.
2001; Rosati et al. 2002; Hasinger et al.
2001) deep surveys have almost resolved the entire 2-10keV X-ray background (XRB), forty years after its discovery (Giacconi
et al. 1962). A large optical follow-up program of
hundreds of X-ray sources in these fields has lead to the
identification of a mixture of obscured and unobscured AGN, with an
increasing fraction of obscured AGN at faint X-ray fluxes (Barger et al. 2003; Szokoly et al. 2004). The optical
counterparts of a significant fraction of the X-ray sources are too
faint ()
for optical spectroscopy, even for
5-6 h exposures with 8-10 m class telescopes. In this work, we focus
on this subsample of X-ray sources with
,
which will be
referred to as Optically Faint Sources (OFS). This criterion
simply reflects an observational limit beyond which we need to rely on
accurate photometric measurements and X-ray spectral information to
estimate their redshift and to establish their physical nature. We
note that OFS represent a quarter of the entire X-ray sample,
therefore they have a significant impact on statistical studies, such
as the X-ray luminosity function, the evolution of the type I/type II
ratio and the overall
distribution. Moreover, many OFS are
relatively bright in the X-ray band, due to powerful AGN activity
(Alexander et al. 2001; Mignoli et al.
2004). It is possible that a sizeble fraction of these
sources belong to the long-sought class of high-redshift, high
luminosity, heavily obscured active galactic nuclei (type II QSOs).
The first detailed study of OFS has been done by Alexander et al. (2001) in the Chandra Deep Field North (CDF-N).
Here we
extend that work by estimating photometric redshifts for a large
fraction of the OFS population, providing direct constraints on their
intrinsic absorption and on their spectral energy distribution.
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Figure 1: Adaptively smoothed Chandra image of the CDF-S in the [0.5-7] keV band. The circles show the position of OFS. The big dashed rectangle is the area of the GOODS survey ( "GOODS area''); the polygon indicates the region of the deep public VLT/ISAAC observations currently available and the small square indicates the area of the Hubble Ultra Deep Field (UDF). |
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The outline of the paper is as follows: in Sect. 2 we describe the X-ray
sample. In Sect. 3 we compare the X-ray properties of the optically bright
(R<25) and faint ()
X-ray sources. In Sect. 4 we derive
photometric redshifts. In Sect. 5 we discuss the few OFS with known
spectroscopic redshifts. In Sect. 6 we use the X-ray to optical flux
ratios as a diagnostic tool. In Sect. 7 we perform an X-ray spectral
analysis and in Sect. 8 we derive the fraction of OFS that are likely to
be X-ray detected type-2 QSOs. We study in detail the OFS inside the
recently released Hubble Ultra Deep Field in Sect. 9. Finally in Sect. 10 we
summarize and discuss the results. Throughout this paper we use Vega
magnitudes (if not otherwise stated) and assume
,
and H0=70 km s-1 Mpc-1.
The X-ray sample is obtained from the 1 Ms Chandra observation
of the Chandra Deep Field South (CDF-S; Giacconi et al.
2002; Rosati et al. 2002). We refer to Table 2
in Giacconi et al. 2002 for the X-ray quantities and
relative errors (e.g., X-ray fluxes, counts). In Fig. 1 we show a smoothed 0.5-7 keV image of the CDF-S
field on which we have highlighted the OFS. The distribution of R band
magnitudes for the X-ray sources is reported in Fig. 2. From the entire X-ray sample of 346 sources, 92
are OFS (), of which 46 (
of the total sample)
do not have a R band counterpart (down to
R=26.1-26.7). In the
CDF-N, the fraction of optically faint sources (
)
is slightly
larger (
;
Alexander et al. 2001);
however, this study was performed in the most sensitive region of the
CDF-N field, while here we are considering the whole of the CDF-S field.
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Figure 2: The R-band magnitude distribution for the optical counterparts of the X-ray sample. The hatched box are the OFS, while the shaded part refers to the sources without a R band counterparts (down to R=26.7). |
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At present only six ()
of the OFS have been
spectroscopically identified, as compared to 151 (
)
of the
optically bright (R<25) X-ray sources (Szokoly et al.
2004). We will discuss in detail the properties of these
six OFS in Sect. 5. For the remaining OFS it
will be challenging to obtain a spectroscopic redshift with 8-10 m
telescopes, with the exception of those sources with strong emission
lines. In order to obtain information on their redshift distribution
we have determined photometric redshifts (see Sect. 4).
Before we investigate in detail the nature of the optically faint X-ray source population, we will compare their general X-ray properties with those of the well-studied optically bright X-ray source population (see also Sect. 4 of Alexander et al. 2001).
In Fig. 3 we compare the X-ray flux distributions
of the optically bright and faint sources in the 0.5-2 keV (left
panel) and 2-10 keV bands (right panel). According to a
Kolmogorov-Smirnov test the probability that the distributions are
drawn from the same population is extremely small (
in
the 0.5-2 keV band and
in the 2-10 keV band).
According to Fig. 3, almost all the bright X-ray
sources are part of the optically bright sample.
The total flux in the 2-10 keV band of the OFS is
erg cm-2 s-1 deg-2 after correcting for the
sky coverage in the CDF-S (see Fig. 5 of Giacconi et al.
2002). This accounts for a
fraction of the
[2-10] keV XRB; the estimated error range corresponds to the
uncertainty in the measurement of the XRB flux (HEAO-1, Marshall et al. 1980 and Revnivtsev et al. 2004;
SAX, Vecchi et al. 1999; XMM-Newton, De Luca &
Molendi 2004).
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Figure 3: The distributions of X-ray fluxes in the 0.5-2 keV ( left panel) and 2-10 keV band ( right panel) for the OFS (hatched histogram) and optically bright sources (open histogram). |
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The hardness ratio (HR) is a useful tool to characterize the spectral
shape of the AGN X-ray continuum. We adopt the definition
HR (H-S)/(H+S), where H and S are the net count rates in
the 2-7 keV and 0.5-2 keV band, respectively. We have recomputed the
HR values over those given in Giacconi et al. (2002) by
performing aperture photometry for each source in both the 0.5-2 keV
and 2-10 keV bands regardless of whether the source is detected in
either of these bands. Therefore, several values previously set to +1 or -1 (Giacconi et al. 2002) have a different value, still consistent with the old one within 1
error. When
,
we plot the 1
upper/lower limits. Other minor
differences come from the new reduction of the CDF-S data performed
after the release of CALDB 2.26 and CIAO3.1. In particular, we applied
the correction for the degraded effective area of ACIS-I chips due to
material accumulated on the ACIS optical blocking filter at the epoch
of the observation using the recently released time-dependent gain
correction (see http://asc.harvard.edu/ciao/threads/acistimegain/).
We have corrected the HR values for the off-axis angle of the source,
normalizing the soft and hard counts to refer to an on-axis source
falling on the aimpoint (chip3). To do that, we have used the soft and
hard exposure maps computed for the monochromatic energies of 1.5 and
4.5 keV respectively.
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Figure 4: The distribution of hardness ratios (HR) for the optically faint sample (hatched histogram) and the optically bright sample (open histogram). |
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In Fig. 4 we show the hardness ratio distributions.
A larger fraction of OFS show a high HR, typical of intrinsically
absorbed AGN emission, than found in the optically bright
sample. The
two HR distributions are distinguishable according to the
Kolmogorov-Smirnov test at the
significance level; a similar
result has been obtained by Alexander et al. (2001) in
the CDF-N. These findings are also in agreement with the general trend
toward flatter X-ray spectral slopes at fainter X-ray fluxes (i.e.
Tozzi et al. 2001). It has been shown that this flattening
is due to the fainter X-ray sources having more absorbed X-ray spectra
(see e.g. Mainieri et al. 2002; Kim et al.
2004).
We conclude that there is a larger fraction of OFS with flat X-ray spectral slopes. To confirm that this flattening is due to high intrinsic absorption we fit the X-ray spectra of each source. We discuss this in more detail in Sect. 7.
Given the optical faintness of the OFS, the only viable way to
determine their redshifts is to use photometric redshift techniques.
In recent years, these techniques have achieved good accuracy,
particularly when high quality multiwavelength imaging data is
available; e.g.
for the Hubble
Deep Field North (Fernández-Soto et al. 1999; Benitez
2000; Furusawa et al. 2000). These procedures
rely on detecting the passage of continuum features within the
spectral energy distribution (SED) of sources across a series of
photometric passbands (e.g., the
break).
Recently these techniques have also been applied to the optical
counterparts of X-ray sources. For these sources the contribution to
the optical/near-IR emission from the AGN nucleus can be significant.
Gonzalez & Maccarone (2002) studied a sample of 65 sources detected by Chandra in the Hubble Deep Field North
and flanking fields. By using a set of galaxy templates, and excluding
objects dominated by the emission from the QSO, they were able to
obtain photometric redshifts to an accuracy similar to that achieved
for non-active galaxies. Mobasher et al. (2004) used the
wide multiwavelength photometry from the Great Observatories Origins
Deep Survey (GOODS)
to derive photometric redshifts for a sample of 19 AGN with
spectroscopic identification. They found an rms scatter of
0.13, good enough to be useful for many science
applications. Finally, Zheng et al. (2004), using the GOODS
photometry, estimated photometric redshifts for the full sample of 346
X-ray sources detected in the CDF-S (Giacconi et al.
2002). By comparison with known spectroscopic redshifts
(137 sources from Szokoly et al. 2004) we derived an
average dispersion
.
In Zheng et al. (2004), we presented photometric redshifts for the full sample of X-ray sources in the CDF-S. In this work, we fully describe our methodology developed to produce the best results for the OFS. By determining likelihood contours in the redshift vs. template plane, our approach clearly elucidate degeneracies/dependencies between redshift and SED/reddening which often affect the photometric redshift determination.
A key ingredient for deriving reliable photometric redshifts is broad,
multi-wavelength coverage and accurate photometry. An area of 160 arcmin2 of GOODS/CDF-S has been imaged with the Advance Camera
for Surveys (ACS) on board of the Hubble Space Telescope (HST) in the
F435W, F606W, F775W and F850LP bands (Giavalisco et al.
2004). A large program with the VLT is under way to
image the GOODS area in the
bands, using some 32 ISAAC
fields to mosaic a 150 arcmin2 region (Vandame et al. in
preparation)
; in addition,
an extensive spectroscopic campaign has been completed with FORS2 at
ESO (Vanzella et al. 2004) and additional spectroscopy
with VIMOS is planned in 2005
. The CDF-S has also been selected
as one of the target fields in the Spitzer legacy program GOODS
(Dickinson et al. 2002). For an overview of the
available data in this field we refer the reader to Giavalisco et al.
(2004).
We will restrict our photometric redshifts
estimation only to the region of the CDF-S covered by deep HST/ACS
imaging (see Fig. 1) and we will refer to it as the
"GOODS area''. In this region there are 192 X-ray sources, 112
of which have a spectroscopic redshift (Szokoly et al.
2004). For this sample we have built a multicolour
catalogue in B435, V606, i775, z850, J, H, bands. For the four optical bands we refer to the publicly available
GOODS catalogue
, while
in the near-IR we use the deep VLT/ISAAC observations (Vandame et al.
in preparation), when available, or the shallower NTT/SOFI imaging
(Vandame et al. 2001).
We used SExtractor (Bertin & Arnouts 1996) for source
detection in each band. To obtain reliable source colours the spread
in seeing conditions for images in different wavebands has been taken
into account. We obtained PSF-matched magnitudes as follows: 1) we
computed aperture magnitudes in each waveband using the available
images ("original'' images); 2) we degraded the point spread function
(PSF) of each image to match the worst condition ("degraded'' images);
3) we recomputed the aperture magnitudes using the "degraded'' images;
4) we derived corrections for the different seeing conditions by
comparing the magnitudes of "bright'' stars in the "original'' and
in the "degraded'' images. These corrections (0.1 mag)
are applied to the "original'' magnitudes. We checked that those
corrections are constant over a large magnitude range. We also
corrected for Galactic extinction: the values in the different filters
have been obtained from the NASA/IPAC Extragalactic Database which are
taken from Schlegel et al. (1998). The corrections in
the CDF-S region are small (from
0.03 mag in the B band to
0.003 mag in the
band).
In the following, we adopt an X-ray based classification as suggested
by Szokoly et al. (2004), but using unabsorbed
luminosities and intrinsic absorption as opposed to uncorrected
luminosities and hardness ratio (see Tozzi et al. 2005).
We introduce the following classes: X-ray unabsorbed QSO:
erg/s and
cm-2; X-ray unabsorbed AGN:
erg/s and
cm-2; X-ray absorbed QSO:
erg/s
and
cm-2; X-ray absorbed AGN:
erg/s and
cm-2; galaxy:
erg/s
and
cm-2.
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Figure 5:
Comparison of the photometric and spectroscopic
redshifts of the spectroscopically identified OFS in the "GOODS
area''. Left side: best fit template (continuum line) with
the observed photometry (filled circles with error bars) and the
best fit model photometry (filled squares) overplotted. Right
side: confidence contours (![]() ![]() ![]() |
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Figure 6: As in Fig. 5. |
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Using the extraordinarily deep and wide photometric coverage in the
"GOODS area'', we have computed photometric redshifts for the OFS.
This allows us to estimate the redshift distribution of OFS to a
greater precision than has been performed before. For example,
Alexander et al. (2001) assumed that most OFS reside in
host galaxies to infer that the majority of the
population is in the redshift range of
.
We used the
publicly available code BPZ (Benitez 2000). This code
combines
minimization and Bayesian marginalization, using
prior probabilities to include a priori knowledge of the
distribution of galaxy magnitudes and spectral types with redshift. We
used the default library of spectral templates in BPZ: four (E, Sbc,
Scd, Irr) are spectral energy distributions from Coleman et al.
(1980) and two are derived from spectra of
starburst galaxies in Kinney at al. (1996). We allowed the
code to calculate two interpolated SEDs between each pair of these
templates.
BPZ provides the "odds'' parameter to characterize the
accuracy of the redshift estimation. This parameter is defined as the
integral of the redshift probability distribution within the interval
,
where
is the value which
maximizes the probability distribution and
the observed
rms. A low value (<0.6) of the odds parameter is a warning that
the probability distribution is spread over a large redshift range or
is double-peaked.
The reliability of the OFS photometric redshifts was estimated using
the five spectroscopically identified OFS in the "GOODS area'':
CDF-S/XID 45, 117, 263, 265 and 606 (see Table 3
and Figs. 5-6).
In the left column the best fit template is plotted together with the
observed photometry. On the right column, likelihood contours
(,
,
)
are reported in the SED
template vs. redshift plane. In all of the five cases the agreement
between the photometric and spectroscopic redshift is extremely good,
even for source CDF-S/XID 117 for which we do not have reliable
near-IR photometry. Therefore we are confident that we can apply this
procedure to the whole OFS class. In Tables 1
and 2 we report the derived photometric
redshifts and the 1
confidence range. Best fits and
confidence contours for each source are shown in Fig. 7.
We have also used X-ray information to set
a posteriori constraints in the redshift solution space. In a plot of
the Hardness Ratio versus the X-ray luminosity of the sources in
the CDF-S (see Fig. 10 of Szokoly et al. 2004) almost
all of the sources spectroscopically identified as AGN have:
and
erg s-1.
Consequently for all the objects with
we have imposed a
minimum X-ray luminosity limit (
erg s-1) that converts to a minimum redshift for each
source (
). In the confidence contour plots the shaded
area corresponds to
,
where the probability to have
the correct solution is low (see Figs. 5
and 7)
.
We compare in Fig. 9 the redshift distribution
of optically bright sources and OFS. We use the spectroscopic
redshift, if known, or the derived photometric redshift, if the source
is still unidentified. The solid histogram shows the redshift
distribution of the OFS, the hatched histogram shows the distribution
of optically bright sources, and the open histogram shows the
distribution of the whole X-ray sample. We have excluded sources
belonging to the two large scale structures at z = 0.67 and 0.73 discovered by Gilli et al. (2003) in the CDF-S. The
uncertainties in the photometric redshifts are too large to determine
whether a source belongs to these structures. Since
of the
spectroscopically identified sources with
belong to the redshift spikes, we assumed that a similar
fraction of sources with
are part
of the same structures.
Table 1: Photometric redshifts for Optically Faint Sources in CDF-S/GOODS.
Table 2: Photometric redshifts for Optically Faint Sources in CDF-S/GOODS.
Table 3: OFS with a spectroscopic redshift in the CDF-S.
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Figure 7:
Photometric redshifts for OFS in the "GOODS area'' with
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Figure 7: continued. |
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Figure 7: continued. |
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Figure 7: continued. |
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Figure 7: continued. |
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Figure 7: continued. |
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Figure 7: continued. |
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Figure 7: continued. |
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Figure 7: continued. |
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Figure 8: X-ray spectrum of source CDF-S/508 with a significant feature that we identify with the Fe line at rest-frame 6.4 keV. |
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In Fig. 9, we have overplotted for comparison the prediction of a synthesis model for the XRB (model B from Gilli et al. 2001).
The majority of the OFS lie at z=1-3, with a small fraction at
z>3, as previously predicted by Alexander et al.
(2001). Perhaps surprisingly, a small fraction of OFS
lie at z<1. We note that a larger fraction ()
of OFS are at
z>1 than found for the optically bright sources (
). According
to a K-S test the probability that these two distributions are drawn
from the same population is extremely small (
).
These have to be taken into account when comparing the redshift
distributions of recent deep Chandra and XMM-Newton
surveys with XRB synthesis models predictions. Almost all of the
spectroscopically identified sources in the two deepest Chandra
pointings are optically bright:
both in the CDF-S and
CDF-N. It has been noted (Hasinger 2002; Gilli
2004) that the redshift distribution of these new surveys
is in disagreement with XRB models predictions based on the ROSAT
X-ray luminosity function. These models predict that the distribution
peaks at
,
whereas the observed N(z) of the sources
identified to date peaks at
.
Since OFS appear to have a
N(z) peaking at
(Fig. 9) and they
make up the majority of still unidentified sources, the disagreement
with the models predictions is attenuated. Nevertheless, a significant
discrepancy with the models remains even with the addition of
photometric redshifts (Fig. 9). A solution for
this problem requires a new determination of the X-ray luminosity
function of AGN (one of the main input parameters of XRB synthesis
models), particularly exploring the X-ray fainter regime not covered
by previous surveys (Gilli 2004). A similar result has been
recently found by Fiore et al. (2003) using a different
approach to derive the redshift information for unidentified sources
in the HELLAS2XMM 1dF sample.
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Figure 9: Distribution of redshifts (spectroscopic and photometric) for the OFS (shaded histogram), optically bright sources (hatched histogram) and the total X-ray sample (open histogram). Sources belonging to the large scale structures in the CDF-S have been excluded (see text). The dashed line is the redshift distribution predicted by the model B of Gilli et al. (2001) normalized to the total number of sources in the "GOODS area'' for which we have either a spectroscopic or photometric redshift. |
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Figure 10:
R-K colour versus redshift. Following the X-ray
classification (Szokoly et al. 2004) described in
Sect. 4.1: circles are X-ray unabsorbed
AGN/QSOs, squares X-ray absorbed AGN/QSOs, triangles
galaxies. Filled symbols refer to OFS, empty symbols to
optically bright sources. The numbers are the XIDs of OFS
spectroscopically identified in the CDF-S (see Table 3). The four evolutionary tracks correspond
to an unreddened QSO (solid line; Vanden Berk et al. 2001),
and to unreddened elliptical, Sbc and irregular galaxies from
the Coleman et al. (1980) template library (dashed
lines). The bars indicate 1![]() |
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Figure 11:
The Hardness ratios (HR) versus X-ray-to-optical flux
ratios (X/O). Open symbols indicate optically bright (R<25)
sources and filled symbols indicate OFS. Symbols are as in Fig. 10. For clarity, we have omitted optically bright
objects that are spectroscopically unidientified. Vertical lines
are for
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Figure 12:
Intrinsic ![]() |
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Finally, a significant fraction (46 out of 346, )
of the
X-ray sources in the 1 Ms Chandra exposure (Giacconi et al.
2002), are not detected in deep VLT optical images down
to
.
Yan et al. (2003) identified in
the near-IR six of these objects using the first release of deep
VLT/ISAAC
data, which covered an area 2.5 times smaller
than the new extended ISAAC imaging shown in Fig. 2. Using optical/near-IR color-color diagrams the
authors concluded that they were likely to be E/S0 galaxies at
.
Taking advantage of the deep optical ACS photometry we
can now set tighter constraints on the redshift of these six sources:
CDF-S/XID 201 has a spectroscopic redshift of z=0.679 (Szokoly et al. 2004)
; the best fit SED of CDF-S/XID 79 and CDF-S/XID 221 is an
unreddened early-type galaxy with redshift
1.821.761.86 and
respectively and the remaining three sources
(XID/CDFS 515,561,593) are best fitted with the template of a spiral
galaxy and have photometric redshifts of
,
and
respectively.
The objects with extreme X-ray-to-optical ratios (EXOs) studied by
Koekemoer et al. (2004) are also included in our sample.
These sources were selected to be undetected in the ACS z band of the
GOODS survey. In this work, by supplementing the HST imaging with new
deep VLT/ISAAC data in J, H and
bands we can improve the
photometric redshift accuracy. Since in several bands we have only
upper limits, the confidence contours for these sources are generally
large and the low value of the odds parameter reflects the uncertainty
in the redshift determination. However, in three cases we have
odds
0.6. The first, CDF-S/XID 243 has a single solution at
high redshift (
,
which gives an absorbed
erg s-1, see Fig. 7) and is best fitted with the SED of an
irregular galaxy. Instead CDF-S/XID 508 has a double solution, with
the peak of the redshift distribution corresponding at
(absorbed
erg s-1) but
with a secondary peak at lower redshift (
2.4, absorbed
erg s-1). We have inspected the
X-ray spectrum of this source, and have detected a clear feature
which, if identified with the Fe line at rest-frame 6.4 keV, would
indicate a redshift of
.
We therefore suspect that the
lower redshift solution is correct. Finally, CDF-S/XID 583 is
detected in the v, i and z ACS bands
and this favours a low redshift solution (
,
absorbed
erg s-1). These results
do not exclude the high-redshift (z=6-7) AGN scenario proposed by
Koekemoer et al. (2004) for a small fraction of the
EXOs population. We conclude that using the best multiwavelength
imaging data set available to date, we have found a candidate at
;
the other two EXOs are most likely at lower redshifts
(
). Forthcoming Spitzer observations of this field shall
determine more accurate photometric redshifts for the EXO population.
For the few OFS with known redshifts, we can study their X-ray
spectral properties. In the CDF-S, there are six of these objects and
we report in Table 3 their main X-ray and optical
properties. The depth of the 1 Ms CDF-S data enables us to perform
an X-ray spectral analysis of these sources. We adopt a power-law
model plus an absorption component. The fit yields the power-law
photon index ,
the intrinsic column density
,
and
the X-ray luminosity in the [0.5-10] keV rest-frame band corrected for
absorption. We give the results of these fits in Table 4. Adopting the X-ray classification
presented in Sect. 4.1, the sample comprises
three X-ray absorbed QSOs, and three X-ray absorbed AGNs.
The identified OFS show a variety of optical classes in Table
3. Following the optical classification introduced
by Szokoly et al. (2004), there are: three
objects showing high excitation narrow lines (C
IV
1549) together with narrow Ly
emission (HEX),
CDF-S/XID 54,117,263, and three objects showing only low excitation
lines (LEX) either Ly
,
CDF-S/XID 45, or [O
II]
3727, CDF-S/XID 265,606. For the sources in the LEX
class, the presence of an AGN is only revealed by their high X-ray
luminosities.
In strongly absorbed X-ray sources, the host galaxy
dominates the optical and near-IR emission. The R-K versus zdiagram can be used to contrain the nature of the X-ray sources. We
present this diagram in Fig. 10 for all of the CDF-S
sources with spectroscopic redshifts, highlighting the OFS. For
comparison, we also plot the evolutionary tracks expected for
classical type-1 QSOs and galaxies of various morphological
types. The optically faint X-ray population has on average redder
colours than the optically bright population. For the 92 OFS of our
sample, we find that 60 ()
of them are Extremely Red
Objects (EROs),
,
as compared to only 28 (
)
for
the optically bright population (see also Alexander et al.
2001 and 2002). The OFS with
spectroscopic identification cover a wide redshift range (z=1-4).
In Fig. 10, we plot also the OFS for which we have
determined a photometric redshift. Almost all of them have colours
dominated by the host galaxy (elliptical or spiral) and, except for a
few candidates at high redshift, the bulk of them lie in the redshift
range of
,
filling in a region that is
poorly sampled by spectroscopically identified X-ray sources.
X-ray-to-optical flux ratios (X/O) can yield important information on
the nature of X-ray sources (Maccacaro et al. 1988). A
value of
is a clear sign of AGN activity since
normal galaxies and stars usually have lower X-ray-to-optical flux
ratios. In Fig. 11, we show the hardness ratios
(HR) versus X/O for the X-ray sources in the CDF-S area. The majority
of X-ray unabsorbed and X-ray absorbed AGN/QSOs are inside the well
defined locus of active galactic nuclei (
), while
"normal'' galaxies, for which the contribution to the X-ray flux is
mainly due to star-formation activity, have
.
The OFS have
ratios characteristic of AGN and
of them show
intriguingly high values (
)
. In
the spectroscopic follow-up of the CDF-S, three of the OFS with high
X/O have been identified (Szokoly et al. 2004; Vanzella
et al. 2004): CDF-S/XID 45,54 and 265 have redshifts of
z=2.291, 2.561 and 1.215, respectively. Two of them are classified as
X-ray absorbed QSOs and one as X-ray absorbed AGN (see Table 3). Recently, Mignoli et al. (2004)
have studied a sample of eleven hard X-ray selected sources with
using deep near-IR observations with ISAAC. All but one of
the sources have been detected in the
band with very red
colors (
). They were able to provide a
morphological classification and the sample is dominated by elliptical
profiles (7/10). Using the morphological information and the R-K colour the authors determined a minimum redshift for the sources in
the range
.
In the OFS inside the "GOODS
area'' there are 20 objects with such high X/O values and we have
determined photometric redshifts for them. Three sources (CDF-S/XID 133,523,614) have extremely low value of the odds parameter and we
will exclude them in the following analysis. Two different classes of
objects are present. Twelve (
)
have a best fitting SED
of an elliptical galaxy, the average column density is
cm-2 and their predicted redshift range is
(with a mean redshift of
1.9). The
remaining sources have a best fitting SED of either an irregular or
starburst galaxy, with a mean redshift of
and X-ray spectra
indicating a low value of absorption (
cm-2). One of these sources is the z>7 candidate
(CDF-S/XID 243)
.
Summarizing,
of
the OFS with
are X-ray absorbed AGN and their
photometry is well reproduced by an unreddened early-type template at
0.9<z<2.7. The other
of the sources do not show
strong X-ray absorption, they have bluer colours and among them there
are some high redshift X-ray unabsorbed/absorbed QSOs.
Finally, a significant fraction (
)
of the sources with
high X/O are X-ray absorbed QSOs.
To further investigate the characteristics of the OFS we have
performed an X-ray spectral analysis of our sample. We use the X-ray
data accumulated in the 1 Ms Chandra exposure and XSPEC
(v11.1) for the fitting procedure. The spectral model adopted is a
power-law with an intrinsic absorber at the source redshift. An
additional photoelectric absorption component is fixed to the Galactic
column density in the CDF-S region of the sky (
cm-2). For sources with less than 100 net counts in the [0.5-10] keV band, we fix the photon index
at 1.8 and derive the
column density
(see Tozzi et al. 2005). To
estimate the intrinsic absorption that is affecting the X-ray source,
its redshift is needed: we use the spectroscopic redshift if known
otherwise we adopt the photometric redshift (Table 1). Thus, we are able to estimate the
value for 336
(
)
of
the 346 X-ray sources in the CDF-S. We show in Fig. 12 the derived
distribution. The
open histogram is the distribution for optically bright sources while
the hatched histogram refers to OFS. A K-S test of the two
distributions gives a probability of
that they are
draw from the same population. We have already deduced from other
diagnostics (X/O, hardness ratios, optical/near-IR colours) that a
large fraction of these faint sources are absorbed. Figure 12 confirms and reinforces this picture
since, in this case, we are measuring directly the absorption from the
X-ray spectrum. Of the OFS
have a column density larger
than 1022 cm-2; for comparison the fraction of bright
sources with such high
value is
.
X-ray
unabsorbed sources (the first bin in Fig. 12) are approximately three times more
numerous among the optically bright than the optically faint
sources.
As mentioned in Sect. 5, a fraction of OFS
could be made of X-ray absorbed QSOs. We find that 11 ()
of the OFS for which we have computed photometric redshifts have
an X-ray luminosity in the [0.5-10] keV band larger than 1044 erg s-1 and a
cm-2, and consequently X-ray
absorbed QSOs according to our definition in Sect. 4.1.
Several synthesis models of the XRB require a large population of
obscured QSOs. To compare our results with the Gilli, Salvati &
Hasinger (2001) and Ueda et al. (2003) models, we
need to use the following definition of a X-ray absorbed QSO:
rest-frame
keV
] > 1044 erg s-1 and
cm-2. We find that 44 sources of the 336 X-ray
sources (optically bright and faint) for which we were able to
determine
,
satisfy these criteria. These X-ray absorbed
QSOs contribute to the [2-10] keV XRB for a fraction of
(if we adopt the HEAO-1 measure of the total flux of the XRB in the
[2-10] keV band)
. Model B of Gilli et al. (2001) predicts a
contribution from type II QSOs to the hard XRB, while
the recent model by Ueda et al.
(2003) requires a lower contribution from these sources
(
)
in good agreement with what we have found.
The Hubble Ultra Deep Field (UDF) is a 400-orbit program to image one
single field inside the "GOODS area'' with the ACS camera on board of
HST (see Fig. 1). Images have been taken in the
same four filters that were used for the GOODS survey: F435W ( b), F606W (v), F775W (i) and F850LP (z). The data
have been recently released and go 1.0 and 1.2 mag deeper
than GOODS in the b and z band,
respectively.
Inside the UDF
area there are sixteen X-ray sources in the Giacconi et al.
(2002) catalogue and three of them are OFS: CDFS/XID
79,515,605. We have extracted cutouts for
these faint sources in the four UDF bands and show them in Fig. 13. The unprecedented depth and resolution
of these images allows us to observe the optical properties of OFS
with sub-arcsecond resolution. We indicate in the cutouts the 3
positional error circle obtained in Giacconi et al.
(2002), which takes into account the strong effect of
off-axis angle in the X-ray PSF and centroid. For CDFS/XID 79 two
different counterparts are clearly present. We name these sources 79A
and 79B (see Fig. 13). They have
different colours: 79A is undetected in the b band and is
brighter than 79B in the i and z bands. In the cutouts of
CDFS/XID 515 there is only one optical counterpart inside the Chandra
error circle. Finally, for CDFS/XID 605 we find three optical
counterparts (A, B, C) of which two are extremely faint in all four
bands (B and C). We have selected from the publicly available
catalogue of the UDF (h_udf_wfc_V1_cat.txt) source magnitudes in
the four bands for each of the optical counterparts. The magnitudes
available from this catalogue where computed using the i band
isophotes of each source, thereby producing isophotally matched
magnitudes that are suitable to compute colours. Combining these
colours with our near-IR photometry, we estimated photometric
redshifts as decribed in Sect. 4.2 (Fig. 14). We provide individual notes on each source
below.
Source CDFS/XID 79: the A counterpart is well fitted with an
early-type SED at redshift
,
similar to that
obtained using the GOODS photometry (see Fig. 7). However, we could not obtain a reasonable
fit to source 79B, probably because the near-IR photometry (which does
not resolve the two counterparts) is dominated by 79A.
Source
CDFS/XID 515: we obtain
and the confidence
contours are in good agreement with the value found with the GOODS
photometry (see Fig. 7).
Source CDFS/XID
605: in this case the depth of the UDF data is really a step forward
for the redshift determination. With the GOODS photometry we obtained
a "double'' solution with a peak in the probability distribution at
low (
)
and high (
)
redshift (see Fig. 7). With the UDF data we
have smaller errors on the photometry and can put a more stringent
upper limit in the b band where CDFS/XID 605 is undetected: this
source is now a strong candidate at high redshift with
,
with a small uncertainty (
4.21-4.32).
Table 4: X-ray spectral parameters of OFS with a spectroscopic redshift in the CDF-S.
![]() |
Figure 13:
Cutouts in the four UDF filters ( F435W, F606W, F775W,
F850LP) with X-ray contours of the three OFS inside this area.
Images are 3
![]() ![]() |
Open with DEXTER |
![]() |
Figure 14:
Photometric redshifts for the counterparts of OFS in
the UDF area. Left side: best fit template (solid line),
the observed photometry (filled circles with error bars), and the
best fit model photometry (filled squares). Right side:
confidence contours (![]() ![]() ![]() |
Open with DEXTER |
In this paper, we have taken advantage of the unique multi-wavelength
coverage of the GOODS survey in the Chandra Deep Field South to
constrain the nature and redshift distribution of optically faint
X-ray sources (). It is important to study their properties
since they are a significant fraction (
)
of the whole
X-ray sample.
Our study extends the earlier analysis by Alexandet et al. (2001) by determining photometric redshifts for the
optically faint sources without spectroscopic redshifts. The
reliability of these photometric redshifts has been tested against the
spectroscopic redshifts available for the optically faint fources (see Fig. 5). We find that a larger
fraction of the optically faint ()
sources are at redshift z> 1 compared to the optically bright sample (
). This finding
reduces the disagreement between the observed redshift distribution in
Chandra deep fields (Barger et al. 2003; Szokoly et al. 2004) and that predicted by XRB models based on the
ROSAT X-ray luminosity function, as the majority of the still
unidentified X-ray sources in these deep fields are optically faint.
However, the redshift distribution that we obtain including our best
photometric redshifts still peaks at
,
while the current
XRB models predict
.
One solution would involve
implementing a new X-ray luminosity function for AGN in the XRB
synthesis models, by combining Deep Chandra and XMM-Newton
fields with shallower surveys (Gilli et al. 2004; Fiore et al. 2003). This new X-ray luminosity function will be able
to reproduce better the evolution with redshift of Seyfert-like
objects which make a large fraction of the observed peak at
.
Several diagnostics indicate that the majority of the optically faint
sources are absorbed. Their hardness ratio distribution is harder
(
significance level) than that of the optically bright sample
indicating a large fraction of optically faint fources with a flat
X-ray spectrum which implies intrinsic absorption. Their
optical/near-IR photometry is dominated by the emission of the host
galaxies and their colours are in average redder that the optically
bright sources (
are EROs, (
)
as compared to
of
the optically bright sources). We have performed an X-ray spectral
analysis and the distribution of
values shows that
of OFS have column densities larger than 1022 cm-2(for optically bright sources the fraction is of
).
We find that
of the optically faint X-ray sources are
X-ray absorbed QSOs (
erg s-1 and
cm-2). Synthesis models of the
XRB include a significant contribution from X-ray absorbed QSOs
to the hard XRB (i.e.
for model B of Gilli
et al. 2001). From the CDF-S survey we find a much lower
contribution from obscured QSOs,
.
This difference can not
be ascribed to the remaining fraction of the as yet unresolved XRB:
both the model and observational values are derived assuming the
HEAO-1 measure of the total flux of the XRB in the [2-10] keV band
and the hard XRB has been resolved (using the HEAO-1 value) to the
depth of the CDF-S (Rosati et al. 2002).
Our value is in
good agreement with the prediction ()
based on the recent
model by Ueda et al. (2003).
Approximatly
of the OFS have high X-ray-to-optical ratios
(
).
of them are strongly X-ray absorbed
(
cm-2) and their photometry is
well reproduced by the SED of an early-type galaxy with
.
The remaining
is on average less
absorbed (
cm-2) and has
bluer colours reproduced by irregular or starburst galaxies with a
mean redshift of
4. Among this second group we find a candidate
at redshift
.
Finally,
of the sources with
high X-ray-to-optical ratios are X-ray absorbed QSOs.
Acknowledgements
We are grateful to Narciso Benitez for his assistance with BPZ. We thank the referee, B. Wilkes, for a very detailed and useful report that improved the manuscript. DMA thanks the Royal Society for financial support. PR gratefully acknowledges support under NASA grant NAG5-11513.