A&A 472, 87-92 (2007)
DOI: 10.1051/0004-6361:20077513
C. M. Gutiérrez - M. López-Corredoira
Instituto de Astrofísica de Canarias, C/.Vía Láctea, s/n, 38200 La Laguna (S/C de Tenerife), Spain
Received 20 March 2007 / Accepted 24 May 2007
Abstract
Aims. We aim to identify the nature of several objects previously catalogued as ultra-luminous X-ray (ULX) source candidates.
Methods. Long-slit spectroscopy of the optical counterparts has been carried out.
Results. The eight objects are at higher redshift than their putative parent galaxies.
Conclusions. It is found that these eight previously catalogued ULX candidates, most of them projected in galactic halos are actually background unrelated objects. This result confirms the high degree of contamination present in current catalogues of ULXs.
Key words: galaxies: quasars: general - X-rays: general
Ultra-luminous X-ray sources (ULXs) are point-like objects that are distributed around
nearby (parent) galaxies; from the redshift of their putative parent galaxies and their
X-ray flux, it is possible to estimate their X-ray luminosity
(
1039-1041 erg s-1). The luminosities of ULXs fill a gap between those of accreting compact stars
1038 erg s-1, and those of active galactic nuclei (AGN;
1043-1044 erg s-1). ULXs were discovered by the EINSTEIN satellite and were extensively found
by subsequent X-ray missions such as ROSAT, Chandra and XMM. ULXs are a relatively rare
phenomenon; Ptak & Colbert (2004), analyzing ROSAT data, estimated that only
12% of
galaxies host at least one of such objects. Major efforts from the theoretical and
observational sides have been dedicated to elucidating the still obscure physical
nature of such sources. X-ray variability over short time scales found in some objects
indicates the compact nature of these sources (e.g., Strohmayer et al. 2007). It has been
proposed that ULXs could be due to super-Eddington accretion, supermassive X-ray binaries, or
beamed emission
(King et al. 2001; Körding et al. 2002). Alternatively, ULXs could represent the manifestation of accreting black
holes of intermediate mass (IMBHs) located in the disks or halos of nearby galaxies.
Although there is strong evidence that relates ULXs with star-forming activity (e.g., Gao
et al. 2003), some inactive galaxies seem to host also many ULXs (Watson et al. 2005).
Some ULXs are associated with recent supernovae (Roberts et al. 2003). Observational
progress in this field (and subsequent identification of the most promising IMBH
candidates) requires more observations in the X-ray region (variability studies,
subarcsecond images, and spectra), and identification and
characterization of possible counterparts in other spectral domains (e.g., Abolmasov et al. 2006; Ramsey et al. 2006).
Table 1: Optical and X-ray properties of ULXs. 1-2. main and alternative identification of the ULX candidates analyzed in this work (LM and LB stand for Liu & Mirabel 2005 and Liu & Bregman 2005, respectively); 3-4. X-ray RA (J2000) and Dec (2000) coordinates; 5. Log of the Luminosity in the 2-10 keV band (for object SW78 the quoted luminosity is in the 0.5-8 keV band) assuming that the X-ray sources were at the distance of the parent galaxy; 6-8. identification, morphological type and distance of the parent galaxy; 9. difference in arcsec between X-ray and nominal optical coordinates.
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Figure 1: DSS images centred on the putative host galaxies ( left). The small black squares correspond to a one square arcmin centred on the ULX candidates analyzed in this paper. These regions are expanded on figures to the right. The arrows identify the optical counterpart of the X-ray sources. Small circles are centred on the nominal X-ray position and have radius of 5 and 1 arcsec for ROSAT and Chandra observations respectively. North is up and east to the left. |
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There are several major catalogues of ULX candidates by Colbert & Ptak (2002),
Swartz et al. (2004), Liu & Mirabel (2005) and Liu & Bregman (2005), which constitute a useful
database for conducting statistical studies or analyzing individual objects. One problem
that has been addressed by many authors (e.g., Ptak & Colbert 2004;
Irwin et al. 2004;
Swartz 2006; López-Corredoira & Gutiérrez 2006) is the high degree of contamination by
foreground (stars in our own galaxy) and mainly background (AGN) objects existing in these
compilations. In fact, this contamination can be on average as high as 50%
(López-Corredoira & Gutiérrez 2006). Similar conclusions have been reached by Ptak &
Colbert (2004) and Liu et al. (2006). Analyzing the spatial distribution of ULX candidates,
the contamination seems to be different according to the type of the putative host galaxy.
In fact, Irwin et al. (2004) claim that elliptical galaxies do not host any ULXs with X-ray
luminosities
erg s-1. So,
until direct confirmation of redshift, existing compilations of such objects must be seen
only as ULX candidates. This makes the identification of optical counterparts
essential. There are several reasons why these identifications are difficult: some
hypothetical counterparts are intrinsically faint, angular resolution (in the case of
ROSAT images) is poor, and ULXs usually reside in crowded regions, thus making
identification of the real counterpart ambiguous.
In previous studies (Arp et al. 2004; Gutiérrez & López-Corredoira 2005; Gutiérrez
2006), we have identified and characterized the optical counterparts of about 13 ULX
candidates. We showed that about 50% of the sources listed in the Colbert & Ptak
catalogue (CP02 hereafter) have an optical counterpart 20 mag. So far, nearly all of
them have turned out to be background/foreground contaminants. In general, these studies
are biased towards the identification of objects with the brightest counterparts and
towards objects situated within more isolated environments. ULX candidates embedded in
HII regions offer probably more chances of being real ULXs. However, in these cases the optical
counterpart is surrounded by the diffuse emission, thus rendering identification very
difficult. In such cases the use of Chandra and HST data is mandatory (Ptak et al. 2006). Here, we extend our observational programme with the identification and
characterization of eight new objects.
We select the objects from the catalogue of ULX candidates by CP02 and Swartz et al. (2004). The objects analyzed in this paper correspond to the optical counterparts of the sources IXO 29, 43, 54, 55, 56, 57, and 70 (we follow the same notation as that of Colbert & Ptak), and CXOU J122517.1+181346 (which we denote as SW 78 hereafter). This is the only object taken from the Swartz et al. catalogue. Table 1 summarizes the main properties of such sources and those of their candidate host galaxies. We look for possible optical counterparts to these X-ray sources in the Digital Sky Survey (DSS) plates, the USNO catalogue, and the released Sloan Digital Sky Survey (SDSS) data. For the eight cases considered here, we have identified a single optical source compatible with the X-ray positions. The last column in Table 1 lists the offset between the optical and X-ray coordinates. Figure 1 shows the DSS images with the identification of the optical counterpart.
The observations analyzed here were taken on the 1.93 m OHP and on the WHT
. Table 2 presents a summary of the
observations. The run at OHP was in March 2005; we did long-slit optical spectroscopy
with the instrument CARELEC, whose grating provides a resolution of 133 Å/mm. The slit was 2 arcsec. This instrumental configuration provided a sampling of 1.78 Å and an
effective resolution of 5 Å as measured from arc and sky lines. More details on the
instrumental configuration can be found in the telescope web pages
(www.obs-hp.fr/www/guide/carelec/carelec-eng.html). With WHT we used the ISIS spectrograph
with the grisms R300B and R158R in the blue and red arm respectively. The
observations were carried out in October and November 2006. In November the conditions were
photometric with very good seeing (
0.5 arcsec) and high atmospheric
transparency. The slit width was 1 arcsec. For wavelength calibration
we took a few Cu-Ar and Cu-Ne lamps at the beginning and at the end of the night.
The stability of the wavelength calibration during the night was checked with the main
sky lines. The sampling was 0.86 Å and 1.64 Å in the blue and red arms respectively.
The effective resolution was 3.8 and 8 Å respectively. The OHP and WHT spectra were analyzed
following a standard procedure using IRAF
that comprises bias
subtraction, flat field correction, coaddition of exposures of the same field,
extraction of the spectra and wavelength calibration. We used standard spectroscopic
stars from the catalogue by Oke (1990) to correct for the response of the configuration
to different wavelengths.
Table 2: Observations. 1. identification of the ULXs. 2. telescope and instrument used. 3. epoch of observations. 4. exposure time.
Table 3: Main features in the optical spectra. 1. identification of the ULXs; 2. observed wavelength; 3. spectral line identification; 4. redshift.
The spectra of the optical counterparts show features which allow a clear
identification and characterization. All of them, apart from IXO 43, show the
presence of broad emission lines typical of AGN/QSOs. In the case of IXO 43 the
spectrum shows only narrow emission lines. The position of these main features
is presented in Table 3. Analysis of each spectrum is
presented below.
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Figure 2:
Optical spectra of the counterparts of ULX sources. The y-axis
is the flux in arbitrary units (counts per angstrom). Broad absorption features (obvious
in most of the spectra) centered at ![]() ![]() |
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This is one of the brightest sources in CP02. DSS plates show an object at
RA = 0541
43.4
,
Dec. = +69
20
46.7
(J2000) with SNR in the peak
8 in the red plates. However this object is not listed in the USNO
catalogue.
The spectral features identified allow us to classify the object as an AGN/QSO at
redshift of z=0.8414, so that it is not physically associated with the putative
host galaxy NGC 1961. The real X-ray luminosity of the object is
erg s-1, which is within typical range of values for AGNs.
The X-ray source is situated close to an open arm of the Seyfert galaxy
NGC 4151. There is an object at 1 arcsec from the X-ray position in the DSS plates that is listed in USNO with photographic
magnitudes 18.8 and 18.1 in b and r respectively. This object appears also
in SDSS classified as a red galaxy with ugriz magnitudes of 20.04, 19.20,
18.42, 18.06, and 17.84. This object was first considered by Arp (1997); it was named
NGC4151: 14 by this author and it was found to have a redshift of z=0.24. However, no spectra
were presented in that work. So the spectrum presented here is the first to be published.
The inferred redshift is z=0.2384, a value that confirms the
original estimate by Arp. The
object, then, is not associated with NGC 4151. The value of log OIII/
does not allow this galaxy to be
accurately classified (Veilleux & Osterbrock 1987). There are also some features that seem to be associated with the stellar
continuum (CaH & K, G-band, etc.) at the same redshift as the emission
lines. The actual luminosity needs
to be computed properly according to the real cosmological distance. Doing
that, we obtained an X-ray luminosity of
erg s-1.
An optical counterpart having magnitudes of 19.2 and 17.5 in b and rrespectively is listed in the USNO catalogue at 5 arcsec from the nominal X-ray
position. No other source listed in the USNO is compatible with the
position of the X-ray source, so we tentatively identify this as the optical
counterpart. The same object has been identified in the SDSS as a stellar-type
object denoted by
J122757.20+130232.8 having ugriz 19.89, 19.17, 18.97, 18.85, and 18.84
respectively. The same object is denoted in 2MASS as 12275718+1302327 and has
magnitudes of 16.762, 16.159 and 15.379 in J, H and K respectively. We
identify the broad emission feature at
4646 Å as MgII(
2799 Å), and the narrow emission line at 6184 Å as OII(
3728 Å). The
apparent feature at 5577 Å corresponds to residual subtraction of a sky line.
Using the OII line we determine a redshift of z=0.6586. With this redshift,
we identified also the emission line of NeIII(
3870 Å). The object
then turns out to be an AGN/QSO with a X-ray luminosity of
erg s-1 and an absolute magnitude (without K-correction)
Mr=-24.07.
This ULX is in the halo of the elliptical NGC 4472. There are no sources listed in
USNO in the position of this X-ray source. A close
inspection of the DSS plates reveals the presence of a faint object at
in the peak with position
RA= 12
29
12.9
,
Dec. = +07
57
41.4
,
and then at
3.7 arcsec from the nominal ROSAT position. The
object has also been detected by SDSS with magnitudes ugriz 20.57, 20.66,
20.41, 20.36 and 20.60 respectively, and with coordinates
RA = 12
29
12.88
and
Dec = +07
57
41.7
.
The spectrum is dominated by several broad emission features
typical of an AGN/QSO. These are easily identified as CIV(
1549 Å),
CIII(
1909 Å) and MgII(
2799 Å) at 3735, 4603 and 6758 Å respectively. Another broad feature at 3380 Å is due to OIV(
1402 Å) with possibly some contribution from SiIV (
1397 Å). Based on these identifications, the redshift is z=1.411. This
corresponds to a luminosity distance of 10 200 Mpc; the actual X-ray
luminosity of the object is
erg s-1. We also found the typical doublet of a
strong MgII absorber at 6275 and 6291 Å, giving a redshift for this absorption system
of 1.2446.
We identify the optical counterpart as the source SDSS J122922.15+075332.5.
This source is not listed in USNO. However, as in the previous case, a
faint object is located in the DSS plates at 2.7 arcsec from the ROSAT
position. The two most obvious spectral features are two broad emission lines
at 3529 and 5178 Å that correspond to CIII(
1909 Å) and MgII(
2799 Å) respectively. Based on those identifications, the object is
an QSO/AGN with z=0.849. We also found the narrow emission
line OII(
2471 Å) at 4574 Å. In the red part of the spectrum, we tentatively
identify weak emission in HeI(
3189 Å), OII(
3728 Å)
and NeIII(
3870 Å). With a luminosity distance of 5410 Mpc, the
X-ray luminosity is
erg s-1.
An optical counterpart having r=18.7 mag is located at 2.7 arcsec from the
nominal X-ray position in the DSS plates. No other object is compatible with
the X-ray position. The optical counterpart is identified as the star
J122923.73+075359.2 in the SDSS survey with magnitudes ugriz 19.56, 19.11,
19.04, 19.15, 19.01 respectively. During the preparation of this
work the SDSS
DR5 was released in which the object appeared spectroscopically measured as a
QSO at z=0.8540. Our spectrum is in agreement with this result. In fact, the
most relevant spectral feature is a broad-band emission feature centered at
5165 Å, which corresponds to MgII (
2799 Å) at z=0.845.
Based on this, we identify two possible additional narrow emission lines centered at
6910 Å and 7175 that we identify as OII(3728 Å) and NeIII(
3870 Å). There is also some evidence for the presence of CII and NeIV in the blue
part of the spectrum. The difference in redshift between the broad and the
narrow features could be due mostly to uncertainties in the determination of
the centroid of MgII; in any case, it would correspond to a difference of
3000 km s-1. The X-ray luminosity of the object is
erg s-1. The apparent r-band magnitude (19.04) measured with
SDSS corresponds to
Mr=-24.66 (without K-correction).
The object has been observed in imaging and spectroscopy by the SDSS
collaboration, who labeled it as SDSS J124406.97+113524.3 and classify it as a
QSO. The ugriz magnitudes are 19.48, 19.31, 19.13, 18.96 and 18.86
respectively. However, according to the NED database, the determination of the redshift was uncertain, with
the values z=4.41 and 1.34 depending on the technique and lines used.
There are no sources listed in the USNO compatible with the position of the X-ray
emission. In this case, this is rather surprising because the object is rather
conspicuous in the DSS plates having
in
the peak. The optical counterpart is situated 3.5 arcsec SW of the X-ray
position. We took long-slit spectra of the optical counterpart with the 1.93 m
OHP telescope in March 2005; however the data were very noisy, making
the identification of spectral features very
uncertain. We observed the object again
with the WHT in November 2006 (these are the data presented here). The spectrum shows
a broad emission feature at 3658 Å. Two other fainter and similar features are
found at 4493 and 6545 Å. These allow us to classify the object as an AGN/QSO
and to identify these lines as CIV(
1549 Å), CIII(
Å)
and MgII(
2799 Å) respectively. From the position of the CIV line
(by far the most intense) we obtain a redshift z=1.363. The X-ray luminosity is then
erg s-1.
The object was catalogued by Swartz et al. (2004) and is the only object
with Chandra coordinates considered in this paper. An object coincident with
the X-ray coordinates is listed in the USNO catalogue as having magnitudes
b=18.4 and r=18.6. The object is well above the noise in the DSS plates and
seems to be elongated. We assume this to be the optical counterpart of the
X-ray source. This is the same object discovered by Knezek & Bregman (1998)
as QSO1225+182 with a tentative redshift of z=1.19. An extended object (or
perhaps a couple of close objects) is located at 8 arcsec from the
optical counterpart. The spectrum of the optical counterpart shows three major broad emission lines that
we identify as CIV(
1549 Å), CIII(
1909 Å) and MgII(
2799 Å) respectively. There are two absorption lines at 3433 and
3441 Å that we identify as the signature of a strong Mg II absorber at
redshift 0.2277. From the emission lines, the object turns out to be an AGN/QSO
at redshift z=1.177 (this is the mean value of the redshifts obtained from the
three main lines). The actual X-ray
luminosity is
erg s-1.
In the eight cases considered here, the object identified as the optical
counterpart of the ULX candidate is the only present in DSS plates, the USNO
catalogue or SDSS images compatible with the X-ray position. Liu & Bregman
(2005) have determined that the positional error of Rosat HRI observations are
well described by a two-dimensional distribution with
arcsec.
This is consistent with the differences (
arcsec) we find
between the position of the X-ray sources and their optical counterparts (see
Table 1, last column). The positional accuracy for Chandra observations is
0.6 arcsec (Aldcroft et al. 2001,
http://cxc.harvard.edu/cal/ASPECT/celmon/)
consistent also with the difference between X-ray and optical positions we found
for SW78. This and the fact that all of them turn out to be emission line
galaxies (at least seven of them AGN/QSOs), objects which have relative low
density, gives confidence in these identifications. In fact, a rough calculation
demonstrates that a misidentification for any of the cases of the counterparts
of Rosat sources that have been classified as QSO/AGNs (i.e. IXO 29, 54, 55, 56,
67 and 70) is unlikely. The mean density of QSO/AGNs brighter than mag 20 in random fields
is
17 per square degree (e.g. Croom et al. 2004; López-Corredoira &
Gutiérrez 2004), and assuming a very conservative error in the X-ray nominal
position of 10 arcsec, the probability to have detected at least one AGN/QSO by chance is
<
.
This is certainly an upper limit to the real probability because the
limit in magnitude and positional errors are very conservative. Due to the better
resolution of Chandra observations, a misidentification in the case of SW78 is
even more unlikely. The optical counterpart of IXO 43 has been identified as an
emission line galaxy with r=18.1 and b=18.8 mag in DSS plates. Although
the density of such objects is about an order of magnitude higher than the one
of AGNs (e.g. Ho et al. 1997), a misidentification for this object is also
very unlikely (
).
Burbidge et al. (2006) claim that the number of ULXs identified as QSOs exceeds the background expectations. However, their analysis does not take into account that the total number of galaxies surveyed (most of them without any ULX candidate) is much more larger. The density of QSOs inferred from the identification presented in this paper (and taken into account that only 12% of the galaxies explored by CP02 hosted an ULX candidate) is roughly in agreement with the density of QSOs up to b=19 mag. Optical expected background densities and further discussion on possible anomalies to these densities were given in López-Corredoira & Gutiérrez (2006).
The
actual X-ray luminosities of the objects identified unambiguously as AGN/QSOs are in
the narrow range
erg s-1, which is in the range
typical for AGN/QSOs (e.g. Boyle et al. 1994). The small relative separation
(
35 arcsec), and the similar redshifts indicate that objects IXO 56 and IXO 57 are
physically related, perhaps members of a larger structure.
It is important to stress that these identifications are clearly biased, and likely they are not representative of the nature of the full sample of ULX candidates. In fact, the objects analyzed here belong to the subsample of ULX candidates that are relatively bright in the optical (thus having a higher optical to X-ray luminosity ratio). None of these belongs to the subsample of 25 objects which López-Corredoira & Gutiérrez (2006) assign higher probabilities to be true ULXs. Most of the ULXs unmasked here were found projected on the halo of early-type galaxies and thus reinforce previous claims (e.g., Swartz 2006) that ULXs are absent in this type of galaxies. Including the objects presented here, there are 40 contaminants already identified from the list of 99 objects presented in López-Corredoira & Gutiérrez (2006).
Acknowledgements
Based on observations made at Observatoire de Haute Provence (CNRS), France and at ORM, La Palma (Spain). MLC was supported by the Ramón y Cajal Programme of the Spanish science ministry. Observations were financed by the OPTICON Trans-national Access Programme.