A&A 408, 51-56 (2003)
DOI: 10.1051/0004-6361:20030963
R. Gil-Merino1 - S. Schindler2
1 - Institute für Physik, Universität Potsdam,
Am Neuen Palais 10, 14469 Potsdam, Germany
2 -
Institut für Astrophysik, Universität Innsbruck,
Technikerstr. 25, 6020 Innsbruck, Austria
Received 19 May 2003 / Accepted 17 June 2003
Abstract
We present CHANDRA X-ray and NTT optical observations of
the distant z=0.52 galaxy cluster RBS 380 - the most distant
cluster of the ROSAT Bright Source (RBS) catalogue.
We find diffuse, non-spherically symmetric X-ray emission with
a X-ray luminosity of
erg/s,
which is lower than expected from the RBS. The reason is a bright AGN in the centre of the cluster contributing considerably to the
X-ray flux. This AGN could not be resolved with ROSAT.
In optical wavelength we identify several galaxies belonging to the cluster.
The galaxy density is at least 2 times higher than expected for such a
X-ray faint cluster, which is another confirmation of the weak
correlation between X-ray luminosity and optical richness. The
example of the source confusion in this cluster shows how
important high-resolution X-ray imaging is for cosmological research.
Key words: galaxies: clusters: general - intergalactic medium - cosmology: observations - cosmology: theory - dark matter - X-rays: galaxies
The galaxy cluster RBS 380 is part of a large optical programme to search for strong gravitationally lensed arcs in X-ray luminous clusters selected from the ROSAT Bright Survey (RBS, Schwope et al. 2000), with a predicted probability for arcs of 45%. In addition to the optical images X-ray observations are taken in order to compare masses determined with different methods and to use the X-ray morphology for lensing models. The main goal of this project is to combine X-ray and optical information, together with possible gravitational lensing information, to constrain cosmological models.
The cluster presented here - RBS 380 - is after RBS 797 (Schindler et al. 2001) the second cluster for which we have performed a combined optical and X-ray analysis. The X-ray source RBS 380 was found in the ROSAT All-Sky Survey (RASS, Voges et al. 1996, 1999) and classified as a massive cluster of galaxies in the RBS. RBS 380 is the most distant cluster of this catalogue.
We present here CHANDRA ACIS-I and NTT SUSI2 observations of the
X-ray cluster RBS 380 at z=0.52 and coordinates
,
(J2000).
We find a lower X-ray luminosity than expected from the RBS. The reason is source confusion in ROSAT data - the X-ray emission of the central AGN had been mixed up with cluster emission.
The high galaxy number density in this cluster is in contrast to its low X-ray luminosity. This is another confirmation that optical luminosity is not well correlated with X-ray luminosity, see e.g. Donahue et al. (2001) or the clusters Cl 0939+4713 and Cl 0050-24 for extreme examples of optical richness and low X-ray luminosity (Schindler & Wambsganss 1996, 1997; Schindler et al. 1998).
Throughout this paper we use
H0 = 65 km s-1 Mpc-1,
and
.
The cluster RBS 380 was observed on October 17, 2000 by the CHANDRA
X-ray Observatory (CXO). A single exposure of 10.3 ksec was
obtained with the Advanced CCD Imaging Spectrometer (ACIS). During
the observations the
front-illuminated array ACIS-I was
active, together with the S0 chip of the ACIS-S
array,
although this last one was not used for the data reduction, since
the expected cluster centre was placed on the ACIS-I array. Each CCD in the ACIS-I is a
pixel array, each pixel
subtending
on the sky, covering a total
area of
.
The data were ground reprocessed on February 28, 2001 by the CHANDRA X-ray Center (CXC). The analysis of these reprocessed data was performed by the CIAO-2.2 suite toolkit.
As upgraded gainmaps from preprocessing were available, we used the acis_process_events tool to improve the quality of the level_2 events file. We also corrected for aspects offsets and removed bad pixels in the field. For that we used the provided bad pixel file acisf02201_000N001_bpix1.fits by the CXC. We built the lightcurve for the observation period and we searched for short high backgrounds intervals. We found none, so no data filtering was needed.
Since we are interested in the diffuse emission of the galaxy cluster, special attention has to be paid to the removal of point sources. This extra care is not needed when the count rate is high enough, since the cluster emission can be seen even without any processing. If the number of counts from diffuse cluster emission is low, any not removed point source can induce wrong estimates. In a broadband (0.3-10 keV) image, we applied two different procedures for the detection of sources: celldetect and wavdetect. The latter uses wavelets of differents scales and correlates them with the image; the former uses sliding square cells with the size of the instrument PSF. In general, celldetect works well with well-separated point sources, although a low threshold selection will obviously overestimate the number of point sources. On the other hand, wavdetect tends to include some diffuse emission regions as point sources. For these reasons, a scientific judgment must be applied in order to decide which regions must be identified as point sources. Using a sigma threshold of 10-6 in the wavdetect routine, we found 31 point sources, expecting a probability of wrong detections of 0.1 in the image. Using analogous criteria for the celldetect routine we found no significant differences.
The correction for telescope vignetting and variations in the spatial
efficiency of the CCDs was done by means of an exposure map, using the standard
procedure of the CIAO-2.2 package. The exposure map was generated for an
integrated energy distribution peak. The value of the peak was slightly
different depending on the included region. Selecting the whole effective area
of the ACIS-I array, the peak value was 0.7 keV. If the selected area was only
the region covering the central part of the cluster (a circle of radio
),
the value of the peak was
then 0.5 keV. We used these two values for the reduction and we could not see
any significant change in the final result.
The background correction was done using a blank field background
set acisi_C_i0123_bg_evt_230301.fits provided by the CXC. We
used a blank field instead of a region from the science image,
since one cannot be sure a priori whether a certain region in the
field is free of galaxy cluster emission. The smoothing process
for the final image was done with the csmooth CIAO tool and compared
to the result using the IRAF (Image Reduction and Analysis Facility)
task Gauss (using a
pixels Gaussian) to be sure that no artificial features were created in
the convolution process. We found no significant differences.
The galaxy cluster RBS 380 was observed in optical wavelength with
the New Technology Telescope (NTT) in service mode during
summer 2001. The Superb Seeing Imager-2 (SUSI2) camera was used in
bands V and R. The SUSI2 detector is a 2 CCDs array,
pixels each, subtending a total area on the sky
of
(the pixel size in the
binned mode
is 0.16''/pixel). In order to be able to avoid the gap between
the two chips during the data reduction process, dithering was
applied.
The data reduction was perfomed with the IRAF
package. A total number of 6 images in R band and 3 in V band in
very good seeing conditions (1'') were used in the analysis.
The exposure time was 760 s for each image. For each band, after
bias subtraction, a standard flatfielding was not enough to
produce good results, because the twilight flats provided by the
NTT team contained some stars and the scientific images showed
stronger gradients than the flats. A hyperflat (see e.g. Hainaut
et al. 1998) was built to flat-correct the images. We briefly
describe the hyperflat technique here.
To produce a hyperflat we processed separately the provided
twilight flats and the scientific images, although the procedure
will be analogous in both sets. The technique is to smooth
strongly all the bias subtracted and normalized frames (with e.g. a
Gaussian
pixels).
The result is then subtracted from the
original frames, so one obtains a very flat background, but still
with stars in the images. Smoothing again the result with a
smaller Gaussian (e.g.
pixels) will show all the stars.
One can then mark all these stars in the original frames, median
average them and reject the marked values. Applying this procedure
to the twilight flats set and to the scientific images set, one
obtains a final twilight flat and a final night-sky flat,
respectively. A linear combination of these two yields the final
hyperflat.
Once the images are flatfielded, they can be co-added, resulting in a deep image of the field and free of chip gaps. Note that the whole procedure has to be done for each filter.
![]() |
Figure 2:
Optical R band image of RBS 380 (z=0.52). The total area is
![]() |
The final X-ray image after data reduction (including point sources
removal) is shown in
Fig. 1. We encircle the main cluster emission within a
radius of
centred on the peak of the emission. The count
rate obtained in that area is 0.05 counts/s. We compared this count
rate to the count rate of the same region in the background fields,
finding a value of 0.02 counts/s. We found that this background count
rate was in fact not very sensitive to its position in the field, as
expected. Using a weighted
average column density
cm-2 (Dickey &
Lockman 1990), a Raymond-Smith source model with T=5 keV and the
cluster redshift z=0.52, the derived luminosity is
erg/s. Using slightly lower numbers for the
temperature in the source model (in the range 3-4 keV), reduces
the final luminosity result in only by a few per cent. This is a
relatively low X-ray luminosity for a massive cluster of galaxies.
As the luminosity is so low we were particularly careful with the
background subtraction and the removal of point sources.
The X-ray luminosity is lower than expected from the RBS results. The reason is an X-ray point source centred on the
coordinates
and
.
The
point source is probably an AGN which could not be resolved with
ROSAT and therefore not distinguished from cluster emission. The
AGN is probably the central cluster galaxy. Within a radius of 7''we find a count rate of 0.07 counts/s for this point source.
Using a power law model
with photon index 2, the same column density as for the cluster
and an energy range [0.3-10 keV], the obtained flux for this AGN
is
erg cm2 s-1. This AGN is one of the
galaxies for which the RBS optical follow-up observations (Schwope
et al. 2000) yielded a redshift of 0.52 (see Fig. 7).
In Table 1 we summarise the coordinates, count
rates and luminosities of the AGN and the cluster.
Name |
![]() |
![]() |
Counts [cts/s] | ![]() |
AGN | 03 01 07.8 | -47 06 24.0 | 0.07 |
![]() |
RBS 380 | 03 01 07.6 | -47 06 35.0 | 0.05 |
![]() |
In addition to the main cluster emission within a circle of radius
described above, we found an asymmetric structure extending
to both sides of this main region. If this is cluster emission, it
could indicate that the cluster is not relaxed, but interacting
with surrounding material or/and an infalling galaxy group. In any
case we consider the inferred X-ray luminosity
as an lower
limit for the cluster. Due to the low number of X-ray counts we did not
perform any spectral analysis.
Name | Redshift | Luminosity [erg/s] | band |
Cl 0500-24 | 0.32 |
![]() |
bolometric |
Cl 0939+4713 | 0.41 |
![]() |
bolometric |
RBS 380 | 0.52 |
![]() |
bolometric |
Both V and R images show a high number density of galaxies. The main goal is to find a way of selecting the cluster members in order to determine their number and their spatial distribution. We select cluster members through a colour-magnitude relation, applying it to all the galaxies detected both in V and R bands.
We use the SExtractor
(Source-Extractor) package to build the catalogue for images V and R. First we extract all the objects detected in both images with a
detection threshold of
over the local sky. We show in
Fig. 3 all the detected objects in both bands,
representing uncalibrated magnitude vs. FWHM. In the two plots a
vertical stellar locus is clearly seen at the position of the
expected seeing for each image (
for V and
for R). We consider all objects to the right of these values as
being galaxies. In the V band, many objects lie on the lower left
side of the vertical stellar locus. We think the problem is due to
the low S/N value in the final V image, built with only 3 original
frames.
We select the galaxies present in both images and calibrate the
magnitudes. For the calibration we use data from the SuperCOSMOS
Sky Survey (SSS). We
obtain from the SSS the magnitudes in R and
for two galaxies
in our field (see both marked in Fig. 7). The calibration
for our R filter is straightforward. For our V filter we use the
contained in the SSS. This means that our V filter is not
perfectly calibrated, but the offset does not induce any
difference in our results (since we are interested in the
shape/slope of the colour-magnitude diagram of our galaxies, the
offset induces only a vertical shift of all the objects in the
plot).
![]() |
Figure 4: Galaxies detected in V (upper panel) and R (lower panel) bands. The magnitudes are calibrated using the SSS archive. |
In Fig. 4 we show the selected galaxies in both V and R images. Stars and deficient detections (SExtractor indicates this with different flags) are rejected. The number of galaxies is 452 in the R filter and only 64 in the V filter. This represents a 70% of the total number of objects detected in R and only a 23% of the objects detected in V.
The next step is to cross-check which galaxies detected in the V image were also detected as galaxies in the R image. We find that all the galaxies in V (64) are also present in the R catalogue.
The existence of a relation between colour and magnitude for
early-type galaxies is well known (Baum 1959; Sandage &
Visvanathan 1978). In Fig. 5 we show the
colour-magnitude relation for the selected galaxies. Since the
presence of a red sequence of early-type galaxies is an almost
universal signature in clusters (Gladders et al. 1998; Gladders &
Yee 2000 and references therein) and clusters at
tend to concentrate elliptical galaxies in their central regions
(Dressler et al. 1997), we look for this sequence in our data. We
select only the galaxies below 23rd magnitude as this is our
completeness limit (see Fig. 6 upper panel for
completeness), and we fit the remaining galaxies by a straight
line. Note that this fit is not sensitive to calibration problems,
these induce only a vertical shift in the line. We used a robust
statistical method based on minimizing the absolute deviation,
which is expected to be less sensitive to outliers compared to
standard linear regression (Press et al. 1992).
The result, presented in Fig. 6 lower panel, shows a red
sequence with slope 0.06. According to the predicted slopes for
formation models of galaxy clusters as a function of redshift in
Gladders et al. (1998, see their Fig. 4), this slope is compatible
with a galaxy cluster at z=0.5. This value does not strongly
depend on the cosmology.
This is particulary interesting because we would have
derived a most likely redshift of 0.5 from this
prediction, which is in good agreement with the actual redshift of 0.52.
In Fig. 7 we show the selected galaxies through the colour-magnitude relation, using the R image. We now want to compare the galaxy number density to the distribution of the X-ray emission in the same area. For the number density map, using a blank image of the same size as the optical image, we allocate pixels with value 1 in all the positions where we detected a galaxy, and then we smooth it strongly (i.e. with a 200 pixels Gaussian). We need such a large smoothing Gaussian because of the low number of galaxies finally detected. In this way we obtain the smooth distribution of the galaxies in the field.
From the X-ray image we extracted the contour lines from the squared region shown in Fig. 1 (which corresponds to the observed region in the optical). In Fig. 8 we plot the galaxy number density together with the X-ray contour lines. The main maximum peak in the number density map is shifted by 2 arcmin in SE direction with respect to the X-ray maximum. Nevertheless, galaxies are present close to the asymmetric X-ray features on both sides of the main peak (in N and NE direction). These asymmetric features might indicate the existence of surrounding material interacting with the cluster, e.g. infalling galaxy groups.
The number of galaxies to the limiting magnitude is at least 2 times
higher than expected for a such faint X-ray cluster (using the
number of cluster members detected in an Abell radius of
within the centre of the cluster) but since the detection members
efficiency is not complete due to the V band poor quality, this number
could even be higher. This is another
confirmation that number of galaxies and X-ray luminosity are not well
correlated (see Table 1 for a comparison with other X-ray underluminous
clusters).
![]() |
Figure 7:
Optical R band image of RBS 380 (z=0.52). The total area is
![]() |
![]() |
Figure 8:
RBS 380 galaxy number density in the R band (upper panel) and the
X-rays contours for the same region (lower panel). The circle with radius
![]() ![]() |
The X-ray source RBS 380 was found in the RASS and identified as a cluster of galaxies in the RBS. From the RBS catalogue, the cluster was expected to be very massive due to its inferred high X-ray luminosity. Its redshift z=0.52 makes it the most distant galaxy cluster in that catalogue. Our interest in this object was due to its predicted probability (up to 60%) of acting as a gravitational lens. In fact these observations are part of a broader project that searches systematically for gravitational arcs in different galaxy clusters and combines this optical information with X-ray studies of the same clusters in order to constrain cosmological models and find possible correlations between X-ray and optical properties of them.
With the new CHANDRA imaging we detect a strong X-ray point source
(an AGN) very close to the cluster centre, which could not be
resolved with ROSAT. After subtracting the emission of this AGN,
the remaining diffuse emission is almost one order
of magnitude less luminous than expected:
erg/s.
No previous investigation of the system has been carried out, so
our first aim was to make sure that it is really a cluster of
galaxies. The X-ray CHANDRA
observation shows a non-relaxed cluster of galaxies probably
interacting with surrounding material or/and another nearby
cluster.
From the NTT optical observations we are able to distinguish some
of the cluster members by means of the
colour-magnitude relation for early-type galaxies present in the
cluster, which is a well known signature for almost every cluster
of galaxies. The obtained slope for this red sequence is 0.06.
Using existing predicted slopes for different formation models as
a function of redshift, the most likely redshift for this slope is
,
in good agreement with the measured redshift of 0.52.
We could not detect any gravitational arc in this cluster. This is not surprising as with the low X-ray luminosity the probability for arcs is strongly reduced.
The example of this cluster shows that high-resolution X-ray imaging is crucial for cosmological research. This type of distant galaxy clusters is often used for various types of cosmological applications. Due to source confusion some clusters can have wrong luminosity measurements and hence influence the results. This effect might e.g. artificially flatten the luminosity function for distant clusters.
Acknowledgements
This work has been partly supported by a predoctoral Marie Curie Fellowship to RGM at the Liverpool John Moores Astrophysics Research Institute (Marie Curie Training Site HPMT-CT-2000-00136), by a German Science Foundation grant (WA 1047/6-1) and by the Austrian Science Foundation (FWF P15868). We thank Olivier Hainaut (ESO NTT-Team) for detailed explanations on hyper-flatfielding. We are grateful to Joachim Wambsganss and Axel Schwope for their work in the arc search programme, by which programme the data sets were provided. We also thank Eelco van Kampen for a number of simulations for better understanding our CM diagrams and Robert Schmidt for comments to a first version of this paper. RGM specially thanks Elisabetta De Filippis and Africa Castillo-Morales for time-sharing and useful discussions during this work and the Institute für Astrophysik in Innsbruck for its hospitality.