Issue |
A&A
Volume 507, Number 1, November III 2009
|
|
---|---|---|
Page(s) | 131 - 145 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361/200912177 | |
Published online | 03 September 2009 |
A&A 507, 131-145 (2009)
Large scale structures around radio
galaxies at z
1.5![[*]](/icons/foot_motif.png)
A. Galametz1,2,3 - C. De Breuck1 - J. Vernet1 - D. Stern2 - A. Rettura4 - C. Marmo5 - A. Omont5 - M. Allen3 - N. Seymour6,7
1 - European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748
Garching, Germany
2 - Jet Propulsion Laboratory, California Institute of Technology, 4800
Oak Grove Dr., Pasadena, CA 91109, USA
3 - Observatoire Astronomique de Strasbourg, 11 rue de l'Université,
67000 Strasbourg, France
4 - Department of Physics and Astronomy, Johns Hopkins University, 3400
North Charles Street, Baltimore, MD 21218, USA
5 - Institut d'Astrophysique de Paris, CNRS, Université Pierre et Marie
Curie, Paris, France
6 - Mullard Space Science Laboratory, UCL, Holmbury St Mary, Dorking,
Surrey, RH5 6NT, UK
7 - Spitzer Science Centre, Caltech, 1200 East California Boulevard,
Pasadena, CA 91125, USA
Received 25 March 2009 / Accepted 27 August 2009
Abstract
We explore the environments of two radio galaxies at
,
7C 1751+6809 and 7C 1756+6520, using deep optical and
near-infrared imaging. Our data cover
arcmin2
fields around the radio galaxies. We develop and apply BzK
color criteria to select cluster member candidates around the radio
galaxies and find no evidence of an overdensity of red galaxies within
2 Mpc of 7C 1751+6809. In contrast,
7C 1756+6520 shows a significant overdensity of red galaxies
within 2 Mpc of the radio galaxy, by a factor of
relative to the four MUSYC fields. At small separation (
),
this radio galaxy also has one z >
1.4 evolved galaxy candidate, one z
> 1.4
star-forming galaxy candidate, and an AGN candidate (at indeterminate
redshift). This is suggestive of several close-by companions. Several
concentrations of red galaxies are also noticed in the full
7C 1756+6520 field, forming a possible large-scale structure
of evolved galaxies with a NW-SE orientation. We construct the
color-magnitude diagram of red galaxies found near
7C 1756+6520 (r < 2 Mpc),
and find a clear red sequence that is truncated at
(AB). We also find an overdensity of mid-infrared selected AGN in the
surroundings of 7C 1756+6520. These results are suggestive of
a proto-cluster at high redshift.
Key words: large scale structure of Universe - galaxies: clusters: general - Galaxy: evolution - galaxies: individual: 7C 1756+6520 - galaxies: individual: 7C 1751+6809
1 Introduction
Galaxy clusters are the most massive collapsed structures in the
universe, which make them an excellent tool for investigating
fundamental questions in astronomy. For example, the evolution of
cluster number density depends sensitively upon ,
but
only weakly upon
and the initial power spectrum
(e.g., Eke et al. 1998),
and thus provides strong constraints on
cosmology. Moderate-redshift clusters from well-defined samples
such as the ROSAT Deep Cluster Survey have been
used to
constrain
and
(Borgani
et al. 2001),
while
Stern et al.
(2009)
use the ages of cluster ellipticals to constrain the equation of
state of dark energy. Distant
X-ray luminous clusters provide the best lever arm for such studies,
yet few have been found to date. Because galaxy clusters supply
large numbers of galaxies at the same redshift, they also provide
unique resources to study the formation and evolution of galaxies.
Due to the sensitivity limits of current surveys, it remains
challenging to identify a large sample of high redshift galaxy clusters
using classical optical
and X-ray selection techniques. During the past decade, a new technique
for detecting galaxy clusters at z > 1 has
been to
look at the immediate surroundings of high-redshift radio
galaxies (HzRGs hereafter; Venemans
et al. 2005;
Best
et al. 2003; Kodama
et al. 2007).
Indeed, it is now well established that the host galaxies
of powerful radio sources are among the most massive galaxies in the
universe (Seymour
et al.
2007). At low redshift, radio galaxies are associated with
giant ellipticals (cD and gE galaxies; Matthews
et al. 1964), which are preferentially located in
rich environments. Because they are so massive, radio galaxies are
excellent signposts to pinpoint the densest regions of the universe out
to very high redshifts (e.g., Stern
et al. 2003). For example, this has been shown by
the strong ()
overdensities of Ly
and H
emitters around HzRGs at
(Venemans
et al. 2005,2007;
Miley et al.
2004; Kurk
et al. 2004a), believed to be the progenitors of
rich, local clusters. However, Ly
and H
emitters found in these environments
are small, faint, blue objects likely to be young star-forming galaxies
and probably constitute a small fraction of both the number of cluster
galaxies and the total mass of the cluster.
Table 1: Observations.
Interestingly, overdensities at the highest redshifts often
have a filamentary nature and extend beyond 2 Mpc (Croft et al.
2005). Carilli
et al. (2002),
in a detailed study of filaments in the field of PKS 1138-262,
an HzRG at z=2.1, do not detect any extended X-ray
emission, indicating that this structure has not yet had sufficient
time to virialize. However, Kurk
et al. (2004b) show that some segregation has
occured, with the H
emitters, tracing the more evolved population, more centrally
concentrated than the younger Ly
emitters. Therefore, the missing link between these proto-clusters and
the classical X-ray confirmed clusters found out to
(e.g., Stanford
et al. 2006; Mullis
et al. 2005)
apparently occurs in the redshift range
.
This redshift range is therefore particularly interesting for
identifying clusters at a redshift beyond where the classical selection
techniques are sensitive,
but at a redshift where clusters are already partly virialized with a
core of older, massive galaxies in place.
In this paper, we present the study of the surroundings of two
radio galaxies at .
The next section describes the targets and the multi-wavelength data
available for the two fields as well as how we derive the multi-band
source catalogs.
The third section describes the color criteria we derive to select
candidate massive cluster
members and the results of this selection. The properties of the
cluster member candidates
are discussed in Sect. 4. A study of the AGN candidates found
in the two fields is also presented
in Sect. 5. Section 6 describes possible close-by
companions of one of our targeted radio galaxies,
7C 1756+6520. We discuss the results in Sect. 7. We
assume a
CDM
cosmology with H0 =
70 km s-1 Mpc-1,
and
.
The magnitudes are expressed in the AB photometric system unless stated
otherwise.
2 The data
2.1 Target selection
This work follows on the SHzRG project (Spitzer
High-Redshift Radio Galaxy; Seymour et al. 2007), which was designed to
study a representative sample of 70 radio galaxies at
and their surroundings. SHzRG obtained rest-frame near- to mid-infrared
photometry for this sample using all three cameras on board Spitzer.
From this sample, we selected radio galaxies with
for further
study. From the seven such sources available in the Spring semester of
the Northern hemisphere, we selected the two radio galaxies with
the most supporting data, 7C 1756+6520 (z =
1.48
; RA: 17:57:05.44, Dec.:
+65:19:53.11) and 7C 1751+6809 (z = 1.54;
RA: 17:50:49.87, Dec.: +68:08:25.93). These two radio galaxies were
first published in Lacy
et al. (1992) as part of a sample
of 57 radio sources selected at 38 MHz. That paper presents
high resolution
radio maps of both objects. Their redshifts were first presented in Lacy et al.
(1999).
2.2 Observations and data reduction
2.2.1 Palomar/LFC B-band data
We imaged the two targets using the Bessel B-band
filter of the Large Format Camera (LFC; Simcoe
et al. 2000) on
the Palomar 5 m Hale Telescope (see Table 1). LFC is a
prime
focus, wide-field
optical imager with a well-sampled 24.6 arcmin diameter field,
imaged by an array of six
pixel
back-side
illuminated SITe CCDs. We observed each target
for 6 h in September 2007. The nights were
photometric with an average 1
seeing.
The LFC data were reduced using the MSCRED
package of IRAF, a suite of tasks designed to process multi-extension,
large-format images from the new generation of optical cameras.
Processing followed standard optical procedures. A distortion
correction was applied to each chip, first using the default solution
for LFC, then matching the stars of the USNO-B1.0 catalog (Monet et al.
2003). The
final stacked image was therefore astrometrized to the
USNO-B1.0 reference frame. For photometry, we calibrated the images
using observations of standard stars from Landolt
(1992). We then converted to AB magnitudes using:
.
We derived the
(
)
detection limits using
diameter apertures uniformly distributed over the images and found
limiting
magnitudes of
27.1
(
26.6).
![]() |
Figure 1:
Color-color diagrams for stars from the matched 2MASS/SDSS catalog (
left) and for stars in the two radio galaxy fields (
right). The spectral types of stars in the left
panel were deduced from optical SDSS colors using Finlator
et al. (2000)
criteria. As illustrated by the solid line, stars with a spectral type
earlier than K5 (
|
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2.2.2 Palomar/LFC z-band data
We imaged the radio galaxy fields using the z-band
filter of Palomar/LFC (see Table 1). In
February 2005, we observed 7C 1751+6809 for
60 min under photometric conditions. In August 2005,
we observed 7C 1756+6520 for 135 min but in
non-photometric conditions. The LFC data were reduced using the MSCRED
package of IRAF. The standard reduction process included an iterative
removal of a z-band fringe pattern derived from the
supersky flat as well as the same correction of distortion process
used for the B-band data. The final, stacked images
were astrometrically registered to the USNO-B1.0 catalog. The FWHM
of the final images is
for
both fields.
Because these data were not all obtained in photometric conditions, nor
were these fields covered by the Sloan Digital Sky Survey (SDSS; York et al.
2000),
photometric calibration of the z-band imaging
relied on empirically derived optical through near-IR color relations
for Galactic stars. Matching a portion of SDSS imaging data with the
Two Micron All Sky Survey (2MASS; Skrutskie
et al. 1997), Finlator
et al. (2000) show that stars have a well-defined
optical/near-infrared color locus, mainly determined by spectral type.
We created a 2MASS/SDSS matched catalog of 530 stars with z
< 18 selected in three random extragalactic fields imaged by
both SDSS and 2MASS. Following recent results from the SDSS
collaboration
, SDSS z
band magnitudes are shifted by 0.02 relative to the AB system in the
sense
.
We apply this systematic shift to the SDSS photometry and convert the J
and K magnitudes from 2MASS to AB
magnitudes using the following corrections:
and
.
Using the criteria defined in Finlator et al. (2000)
and optical photometry from SDSS (g, r
and i-band) to separate stars into spectral
classes, we plot their location in a J - K
vs. z - K color-color diagram
(Fig. 1,
left panel). Stars with spectral type K5 and earlier have
J
- K < -0.26 and a color-color relation well
fit by a simple linear function:
.
Galaxies and cooler stars have redder J - K
colors.
Using 2MASS photometry, we identified stars with a spectral
type earlier than K5
in our two radio galaxies fields assuming a
color. We selected 72 and 40 stars, respectively, for
7C 1756+6520 and 7C 1751+6809. Using the above
color-color relation, we thus derived the z-band
photometric zeropoints
for the Palomar data. The color-color diagram for stars in our fields
is given in Fig. 1
(right panel). Measuring the dispersion of the empirical color-color
relation, we estimate a 0.1 mag uncertainty in the z-band
photometric zeropoints. The
(
)
limiting magnitude determined from random
diameter apertures is 25.0 (24.5) for 7C 1756+6520 and 24.8
(24.3) for 7C 1751+6809.
2.2.3 CFHT/WIRCAM data
In order to sample the red side of the 4000 Å break
at the redshift of the targets, the radio galaxies fields were observed
in the J and Ks bands
using the new Wide-field Infrared Camera (WIRCAM; Puget et al.
2004) of
the Canada-France-Hawaii Telescope (CFHT; see Table 1). WIRCAM
contains
four
pixel HAWAII2-RG detectors with a gap of
between arrays, and covers a
field of view (FoV) with a sampling of
per pixel. The imaging observations were obtained in April, May and
July 2006 (Projects 06AF38 and 06AF99; P.I. Omont).
The seeing varied between 0.7 and
during the observations and the nights were photometric.
The WIRCAM data suffer from serious crosstalk, which echoes
all bright objects in the 32 amplifiers
of each chip. Although our HzRGs are at high Galactic latitude (
),
our images contain
numerous bright stars due to the wide field of view of WIRCAM. The
crosstalk has different profiles and thus proves especially challenging
to correct. Several techniques were attempted to correct crosstalk but
none of them were fully satisfactory. For our total exposure time of
approximately 3h30 in the J band, the
crosstalk is clearly visible for all objects brighter than
magnitude 16. In the end, we processed the WIRCAM data without
any crosstalk correction and instead flagged the most seriously
affected regions (see Sect. 2.3). The remaining processing
followed standard near-infrared data reduction strategies. We
subtracted the dark and performed flatfielding with a super flat
created from science frames. The images were then sky subtracted and
stacked using the reduction pipeline developed by the Terapix team
(Marmo
2007). The images were photometrically calibrated to 2MASS J
and K bands using
60 stars per field. The
(
)
limiting magnitudes determined from random
radius apertures in the J and Ks bands
are
24.4 (
23.9) and
23.4 (
22.9),
respectively.
2.2.4 Spitzer/IRAC data
Observations with the Spitzer Infrared Array
Camera (IRAC; Fazio et al.
2004) were performed as part of the GO-1 Spitzer
program ``The Most Massive Galaxies at Every Epoch: a Comprehensive Spitzer
Survey of High-Redshift Radio Galaxies'' (Seymour
et al. 2007). These data consisted of four dithered
30 s exposures in each of the four IRAC channels (see
Table 1).
The size of the final IRAC mosaic is about
.
Due to the configuration of the camera, only a
region is covered with all four bands. The data were processed and
mosaiced using the MOPEX package (Makovoz & Khan 2005) from the
Spitzer Science Center and re-sampled by a factor
of two. The final pixel scale is
(see Seymour et al. 2007 for further details on the Spitzer
data and processing). The
limiting magnitudes determined from random
radius apertures are 22.1, 21.7, 19.8 and 19.7 for the 3.6, 4.5, 5.8
and
m
channels, respectively.
2.3 Catalog extraction
For the WIRCAM data, we identified crosstalk-affected pixels in the J
band image, the deeper of our
WIRCAM bands. A map was created to flag crosstalk contaminated pixels
as well as the zones contaminated by bright star artifacts, which
accounted for approximately 8% of the final mosaic pixels (see
Fig. 2).
The J and Ks images were
smoothed to the
seeing of the B and z band
data. We used SExtractor (Bertin & Arnouts 1996) to extract
source catalogs with SExtractor dual mode for J and
Ks using the unsmoothed images
for object detection and the smoothed one for photometry. For B,
z, J and Ks
bands, we derived colors using a fixed 2
5
diameter aperture. For total magnitudes, we used the Kron automatic
aperture photometry given by the SExtractor MAG_AUTO parameter. All
magnitudes were corrected for Galactic extinction using the dust maps
of Schlegel
et al. (1998)
assuming the RV
= AV/E(B
- V) = 3.1 extinction law of Cardelli
et al. (1989).
Since both fields are at high Galactic latitude, their extinction maps
are very uniform.
For both fields, the applied corrections were 0.18 in B-band,
0.06 in z, 0.04 in J and
0.02 in Ks.
![]() |
Figure 2: Combined field covered by our B, z, J and Ks-band data showing both the weight map of the WIRCAM data (J) and the cross-talk flag map. We also flag regions contaminated by bright stars. The dashed lines outline the regions covered by the four IRAC bands. The positions of the HzRGs in the fields are indicated by stars. |
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The point source function (PSF) of IRAC is well defined (Lacy et al.
2005),
providing consistent and readily tabulated aperture corrections to
determine total magnitudes from aperture photometry. For both
magnitudes and colors, we chose an aperture of 2
5 diameter and corrected the
measured flux by the corresponding multiplicative correction factors -
i.e., 1.68, 1.81, 2.04 and 2.45 for the 3.6, 4.5, 5.8 and
m channels,
respectively.
Combining all of these catalogs, we built a master catalog
which provides multiwavelength
data for all sources detected in at least one of the eight bands
observed. The final surface covered by B, z,
J and Ks and not affected by the
WIRCAM cross-talk is 0.1 square
degrees.
Figure 3
shows the galaxy number counts for the different bands compared with
previous counts from the literature. The galaxies were first isolated
from the stars based on SExtractor parameter CLASS_STAR. The 1
error on the number counts
is overplotted in Fig. 3,
assuming a Poisonnian error.
No incompleteness correction was applied to the counts.
The galaxy counts determined from B, J
and Ks were compared to previous works: Metcalfe
et al. (1995); Williams
et al. (1996);
Metcalfe
et al. (1991) for B, Maihara
et al. (2001); Teplitz
et al. (1999)
for J and Maihara
et al. (2001);
Elston
et al. (2006) for Ks. For the z-band,
we derive number counts from zBoötes (Cool
2007), a z-band survey of the Boötes
field that covers 7.62square degrees and reaches a
completeness limit of 23.4
.
We also derive z-band number counts from the
GOODS-MUSIC catalog, a multiwavelength catalog of Chandra
Deep Field South (CDFS) in the GOODS South field (Grazian
et al. 2006b,
see Sect. 3.1 for details on this catalog).
![]() |
Figure 3:
Galaxy number counts for our B, z,
J and Ks data. We use the
stellar index determined by SExtractor (CLASS_STAR) to separate
galaxies from stars. No completeness correction was applied. The 90%
completeness limits of our images for elliptical and spiral galaxies
are indicated by the two vertical dotted lines. We plot number counts
from the literature (see legends for symbols; GM: GOODS-MUSIC). The
counts in B, z and J
are found in good agreement with the literature. However, the
7C 1756+6520 field shows an excess of sources with
|
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The B, z and J-band
counts are found in good agreement with the literature. The Ks-band
counts
are also found in agreement with previous studies for the field around
7C 1751+6809. The field
around 7C 1756+6520 however shows an excess of sources with
;
at the faint limit, Ks number
counts drop due to incompleteness. This overdensity is the first
evidence of an overdensity of very
red objects around this radio galaxy.
2.4 Completeness
In order to assess the completeness limit of our images, artificial
galaxies of different types were added
to our images using the IRAF artdata package (gallist
and mkobjects routines). We first consider
the completeness limit for elliptical galaxies. For half magnitude
intervals of brightness, we created catalogs of
5000 elliptical galaxies which were randomly added to the B,
z, J and Ks
images, including Poisson noise. We adopted a de Vaucouleurs surface
brightness law, a minimum galaxy axial ratio b/a
of 0.8 and a maximum half flux radius of 1
0.
Running SExtractor with the same configuration files used for the
unadulterated data, we determined the fraction of artificial sources
detected. For ellipticals, the derived 90% completeness limits for our
images are 25.0, 23.2, 22.8, and 22.2 in the B, z,
J and Ks bands,
respectively. We then determined the completeness limit for spiral
galaxies by creating catalogs of 5000 spirals galaxies
assuming an exponential disk surface brightness law with a minimum b/a
of 0.8 and a maximum half flux radius of 1
0.
The derived 90% completeness limits are 24.8, 22.9, 22.6 and 21.7 in
the B, z, J
and Ks bands, respectively. As expected, the
completeness limit for exponential
profile galaxies is slightly worse than for ellipticals due to the less
compact nature of their morphologies.
3
Candidate
massive cluster members at z
1.5
We now consider the environments of 7C 1756+6520 and 7C 1751+6809. We first introduce a color criterion to select candidate cluster members based on the BzK selection technique of Daddi et al. (2004). We then discuss the selection of candidates selected using the full multiwavelength master catalog (Sect. 2.3) and finally present the results on the properties and clustering of these sources.
3.1 Color
selection of evolved galaxies at z
1.5
Substantial effort has gone into identifying color criteria to select
galaxies and galaxy cluster members at high redshift. Selecting
extremely red objects (EROs; ), Stern et al.
(2003) and
Best
et al. (2003)
successfully identified evolved galaxy overdensities around HzRGs at
.
It has been shown that near-IR color criteria can be used to robustly
identify passively evolving galaxies at
.
These criteria are mainly based on the position of the
4000 Å break at a given redshift. Thus, the criterion
,
which was first exploited by the FIRES team (Franx
et al. 2003), is now well established and has been
used to select cluster members at z >
2(Distant Red
Galaxies, hereafter DRGs; Tanaka
et al. 2007; Kajisawa
et al. 2006). The galaxies selected by this
criterion are mainly massive, evolved galaxies with old stellar
populations. The goal of the current study is devise color criteria
that are
optimized for identifying evolved galaxies at
,
sampling slightly higher redshifts than the ERO selection criteria,
but not as high redshift as the DRG or Lyman break selection criteria.
Based on the K20 survey (Cimatti
et al. 2002), Daddi
et al. (2004) proposed a simple two-color criterion
based on BzK-band photometry for identifying
galaxies at
and classifying them as either star-forming galaxies, selected by
(hereafter sBzK galaxies) or passive evolving
systems, selected by
(hereafter pBzK galaxies). The BzK
selection is largely insensitive to dust extinction since E(B-V)
is
parallel to BzK
= -0.2 criterion (Daddi
et al. 2004). This two-color selection is therefore
particularly efficient at isolating the red massive component of galaxy
clusters at
.
We consider first the colors of different stellar populations
at
obtained from the Bruzual & Charlot (2003) models
(Fig. 4).
The different curves show the various dust-free
models predictions
(from left to right,
Gyr),
assuming solar
metallicity and a Salpeter (1955) initial mass function. For each
model, four different population ages are indicated (
t =
2.5, 3, 3.5 and 4 Gyr). As previously stated, the BzK
criterion is relatively insensitive to dust extinction since the
reddening vector for an extinction of
E(B-V)
= 0.2 is almost parallel to the
BzK
= -0.2 line (see black arrow in Fig. 4).
![]() |
Figure 4:
BzK color-color plot of stellar population
models at z = 1.5. The curves account for star
formation histories with various |
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The model colors are consistent with the BzK
selection criterion, with models covering first the sBzK
zone and then the pBzK zone of
the BzK diagram as
decreases. We note however that the criterion is most likely missing
early-type galaxies at z > 1.4, in
particular those
with the youngest stellar populations (models with small
and large t values). We overplot a sample of the
(rare) examples of early-type galaxies at
1.4 < z < 2 and spectroscopically
confirmed in the literature. Daddi
et al. (2004) report five high redshift early-type
galaxies from the K20 survey, classified as such on the basis of
continuum breaks and absorption lines in their spectra. Four are in the
GOODS area and one is in the Q0055 area.
Cimatti
et al. (2008)
used the Galaxy Mass Assembly ultra-deep Spectroscopic Survey (GMASS; Kurk et al.
2008) to
find passive galaxies at z > 1.4. They used
the UV
properties of passive galaxies and derived a color index of the UV
continuum for galaxies with spectroscopic redshift z
>1 (see Cimatti et al. 2008, for details).
Thirteen
passively evolving galaxies at
1.390 < z < 1.981 were found in
GMASS, seven of which are members of an overdensity at
(Kurk
et al. 2008).
The Gemini Deep Deep Survey (GDDS; Abraham
et al. 2004) obtained spectroscopy
for 309 objects attempting to target galaxies in the ``redshift
desert''
(1 < z < 2)
.
Fifty of these sources have BzK photometry (SA12
and SA15 fields) and
,
of which five have BzK
< -0.2. One of these sources is at z
> 2 and
has a z - K which is far too
blue to be considered as a passively evolving galaxy (z
- K < 1). We therefore find only four strong
candidates for passively evolving galaxies in GDDS. The location of all
these passive galaxies in the BzK diagram is given
in Fig. 4.
Nine out of 22 are found to have
z
- K < 2.5. We thus confirm what we had
already suspected from the models, i.e. the BzK
criterion for the pBzK selection is missing a
significant fraction (
40%)
of old galaxies at z > 1.4.
We revise the pBzK criterion and adopt
rather than
,
coupled with BzK
< -0.2, to select passively evolving galaxies at z
> 1.4 (hereafter pBzK* galaxies). This color
cut has
been chosen as a compromise between following the elliptical model
color predictions as well as selecting the majority (
)
of spectroscopically confirmed passive systems at z
> 1.4 to date and minimizing contamination from very red
galaxies at
lower redshift. Rettura
et al. (2008) study a sample of 27 early-type
galaxies found in the CDFS with
1.09 < z < 1.35. Out of 27, only four
(all with z >1.3) are selected with our
extended BzK
criteria (see Fig. 4,
open circles; BzK photometry from A.Rettura,
private communication). We are therefore confident that the
contamination of lower redshift red objects is small. Indeed, since the
4000 Å break is at the red end of the z-band
at
,
the z - Ks color
increases rapidly with redshift for
making this simple color criteria an efficient redshift indicator,
especially for passive systems.
Grazian
et al.
(2006b) presents the GOODS MUlticolor Southern Infrared
Catalog (GOODS-MUSIC), a multiwavelength catalog of the GOODS South
field, combining imaging ACS (optical), VLT (near-infrared), and Spitzer
(mid-infrared) data with available spectroscopic data. Grazian
et al. (2006b)
applied a photometric redshift
code to this multiwavelength dataset.
For this study, we used an updated version of the GOODS-MUSIC catalog
(version 2) recently presented in Santini
et al. (2009). The new catalog contains, among other
things, additional spectroscopic redshifts and new
MIPS
m
photometry. The total area covered by the GOODS-MUSIC catalog is 143.2
square arcmin. We check the revised BzK selection
technique using the photometric redshifts (
hereafter) of the pBzK
(65), pBzK*
(116) and sBzK (4727) galaxies found in the
GOODS-MUSIC catalog. Of the pBzK galaxies, 56% (78%)
are found with
(
). The corresponding
percentages are 49% (74%) for
the pBzK* galaxies and 82% (88%) of the sBzK
galaxies. Using the same photometric redshift code as used for
GOODS-MUSIC
,
Grazian
et al. (2006a)
estimate an accuracy of
for red galaxies (J-K>0.7)
and
for their full sample. Figure 2 of the same paper shows that,
at all redshifts, the photometric redshifts systematically
underestimate the spectroscopic redshifts. Similar results were also
found in Mobasher
et al.
(2004) whose photometric redshifts in the GOODS Southern
Field at z>1.3 were also underestimated. The
percentages presented above are thus likely
lower limits. The revised BzK selection is
therefore very efficient at isolating red galaxies
at z>1.4, with some inevitable contamination
by
lower redshift reddened galaxies.
3.2 Candidate cluster members
The combination of filters used during the observations were checked
for consistency with the one used by Daddi
et al. (2004). Comparing the shape of the filter
transmission curves, we deduce that the B-band
filters are equivalent. The z-band filter of
Palomar/LFC is consistent with the Gunn z-band of
VLT/FORS1 though it is shorter at long wavelength by 400 Å.
Finally, the CFHT/WIRCAM Ks-band filter is slightly
more extended at bluer wavelength (by
300 Å)
compared to the one used at VLT/ISAAC by Daddi
et al. (2004). We use a library of galaxy templates
generated with PÉGASE2 (Projet d'Étude des Galaxies par Synthèse
Évolutive; Fioc & Rocca Volmerange 1997) and compare the colors
obtained with the different filter sets. We conclude that the
correction to the B - z color
is negligible, especially for galaxies at intermediate to high redshift
(
- less than 0.02) and the
correction to z - Ks
color is not systematic (i.e., depending on the galaxy type
and age) and are generally smaller than the calibration error of our z-band
photometry (e.g.
0.1 mag
on average; see Sect. 2.2.2).
We next verify that the depth of our data is sufficient to
select passively evolving systems at z >
1.4. The
magnitudes of early-type galaxies at z > 1.4
and
confirmed spectroscopically are, unfortunately, rarely given in the
literature. Furthermore, the selection of such objects itself is
strongly biased to the brightest objects. We look at the expected
magnitudes of pBzK* galaxies in the GOODS-MUSIC
catalog (see §3.1). 57 objects have
and BzK magnitudes fitting the pBzK*
criteria (hereafter the ``GM sample''). These sources have
24.8 < B < 29.7 (
),
22.2 < z
< 26.2 (
)
and
(
).
Considering the
limits of our imaging, our Ks data would
detect 98% of the GM sample, our z data
would detect 75% of the GM sample, but our B data
would detect only 11% of the GM sample.
Therefore, we treat the z-band as the limiting band
for this work and consider sources with
upper limits in B. However, at a given B
magnitude, fainter objects in z will have a bluer B-z
color, corresponding to bluer objects. We are therefore confident that
the majority
of very red passive members of the clusters will be selected in our
dataset.
![]() |
Figure 5:
Color-color BzK diagram of 7C 1756+6520 at
z = 1.48 ( top) and
7C 1751+6809 at z = 1.54 ( bottom).
The sBzK and pBzK selection
regions defined by Daddi
et al. (2004) are shown by the solid lines. Our new pBzK*
selection is shown by the dot-dashed line. The dashed line separates
stars and galaxies.
All sources with a |
Open with DEXTER |
We select the sBzK, pBzK and pBzK*
galaxies around 7C 1756+6520 and 7C 1751+6809 using
our multi-wavelength catalog. The coordinates and B,
z, J and Ks magnitudes
of the pBzK* galaxies are given in Tables 5 and 6 for
7C 1756+6520 and 7C 1751+6809 respectively. We assume
Poisson errors for source density determinations. Figure 5 shows the BzK
color diagram of all the objects with a
detection in B, z and Ks.
We also plot the sources that have a
but no (or <
)
detection in the B-band (arrows). In order to place
those sources in Fig. 5,
we assign them the
detection limit for the B magnitude (B
= 27.1). For 7C 1756+6520 (7C 1751+6809), we found
129 (106) pBzK* galaxies including 42 (42) pBzK
galaxies (with a
detection in z and Ks). This
gives a surface density of
(
) arcmin-2
for pBzK* galaxies and
(
) arcmin-2
for pBzK galaxies. We extract the star-forming
candidates with a
detection in B, z and Ks
and found 218 (200) sBzK galaxies, i.e., a
surface density of
(
)
arcmin-2. 14 (26) sources have
and no (or <
)
detection in B (green arrows) and can not be
reliably distinguished as star-forming or passive systems.
Considering the J-Ks
color of the BzK sources, there is a clear
difference between sBzK and pBzK
galaxies, with pBzK galaxies having a redder and
narrower distribution centered around
(0.93) for the 7C 1756+6520 (7C 1751+6809) field. sBzK
galaxies have a
(0.57). We note that the pBzK* galaxies found around
7C 1756+6520 are, on average, redder that those found in the
7C 1751+6809 field.
3.3 Surface density of BzK-selected galaxies
We now compare the densities found in our HzRG fields to blank fields. Grazian
et al. (2007)
study the properties of various classes of high redshift galaxies,
including pBzK and sBzK sample in
the GOODS-MUSIC sample. They compare their number densities of sBzK
and pBzK galaxies with the literature (Reddy
et al. 2006; Kong
et al. 2006; Daddi
et al. 2004) and conclude that the GOODS-South field
is representative of the distant universe. We therefore use the
GOODS-South as a first comparison field for our HzRG field. We cut the
GOODS-MUSIC catalog at the same completeness limit as our data,
i.e., we select pBzK and pBzK*
galaxies to our 90% completeness limits of
and z
< 23.2, and we select sBzK
galaxies to
and z < 22.9. The number densities of sBzK,
pBzK and pBzK* galaxies in the
GOODS-MUSIC catalog are given in Table 2
(Col. 2)
assuming Poisson errors on the numbers. The corresponding densities in
our two fields (corrected for incompleteness) are given in
Cols. 8 and 10.
We also compare our results to the MUSYC survey. The MUSYC
survey (Quadri
et al. 2007; Gawiser
et al. 2006)
consists of four fields: an extended Hubble Deep Field South (E-HDFS),
an extended Chandra Deep Field South (E-CDFS) and two fields called
SDSS 1030 and CW 1255. We note that the region
covered by GOODS-MUSIC is included in the E-CDFS.
Optical and near-infrared imaging of
were obtained for all the fields. Deeper near-infared imaging of
were obtained for subfields of SDSS 1030 and CW 1255
as well as for two adjacent subfields of E-HDFS (resulting in a deeper
subfield of
for E-HDFS). The MUSYC team did not obtain additional data for E-CDFS
since the region had already been observed extensively by the GOODS
team. All images and photometric catalogs are available on the MUSYC
website
. We use four
catalogs
of the MUSYC fields i.e., the multiwavelength catalogs of the deepest
subfields in E-HDFS (201.1 sq. arcmin),
SDSS 1030 (106.7 sq. arcmin) and
CW 1255 (101.9 sq. arcmin)
presented in Quadri
et al.
(2007) and the catalog of the full E-CDFS
(969.6 sq. arcmin; Taylor et al. 2009 in
preparation). For each field, we select the pBzK, pBzK*
and sBzK galaxies to the 90% completeness limit of
our data. Surface densities of the MUSYC fields are given
in Table 2
(Cols. 3-6). The surface densities derived from the four MUSYC
fields is given in Col. 7. Since GOODS-MUSIC is in E-CDFS, the
surface densities for those two fields are not independent; see
Table 2,
Cols. 2, 3.
![]() |
Figure 6:
Histogram of the number of pBzK* (red) and sBzK
(blue) galaxies in the MUSYC E-CDFS field in circular cells of
|
Open with DEXTER |
Whereas the star-forming sBzK galaxies only vary by
up to 70% from field to field,
the red pBzK and pBzK* galaxies
show significant field to field variations. The surface densities of
both pBzK and pBzK* galaxies
around 7C 1756+6520 are comparable to the MUSYC
SDSS 1030 field, the denser control field as far as the red
galaxies are concerned. We find an excess of pBzK
and pBzK*
galaxies by a factor of
and
relative to the average density derived from the four MUSYC fields. The
density of sBzK in the full 7C 1756+6520
field is, on the contrary consistent with the control fields. We find
that BzK densities in 7C 1751+6809 are all
in good agreement with MUSYC and GOODS-MUSIC.
![]() |
Figure 7: Ks number counts for pBzK (red), pBzK* (orange) and sBzK galaxies (blue) compared with counts from Kong et al. (2006; K06). The solid and dashed lines correspond to 7C 1756+6520 (1) and 7C 1751+6809 (2), respectively. |
Open with DEXTER |
![]() |
Figure 8:
Spatial distribution of the BzK-selected galaxies
in the two fields: left panels, pBzK*
galaxies
in red with the size of the symbol scaled according to the Ks-magnitude;
right panels, sBzK
galaxies in blue. The radio galaxies are marked by the red stars. The
area simultaneously covered by the BzK bands is
outlined and all sources detected in all three bands ( |
Open with DEXTER |











In order to further quantify the probability to find an
overdensity of pBzK* and sBzK
galaxies in a 2 Mpc radius region, we now work out the
counts-in-cells fluctuations of E-CDFS, the largest field of MUSYC. We
measure the number of pBzK* and sBzK
galaxies (in the limits of completeness) found in
10 000 randomly placed circular cells of
radius (corresponding to 2 Mpc radius at z=1.48)
in the E-CDFS 969.6 sq. arcmin field of view. Edges
were avoided by forcing the cells centers to be at least
distant from the edges of the E-CDFS field. We chose a large number of
cells (allowing some overlapping) to fully sample the counts
fluctuations. We do not consider counts-in-cell of pBzK
in this analysis due to the very small number of these galaxies in
E-CDFS (18). Figure 6
shows the histogram of counts-in-cells. sBzK are
more common than pBzK*.
In order to be able to directly compare those two populations, we
subtract from our counts
the expected average density in E-CDFS scaled to the cell size. Counts
are given in percentage of the total number of cells. We also mark with
arrows the galaxies counts within 2 Mpc of our two HzRGs (also
corrected from the average E-CDFS density).
The histogram has a right-skewed distribution. We note that the tail of
the distribution of red galaxies is longer that the one for blue
galaxies
confirming that red galaxies are more clustered than blue ones
(see Kong
et al. 2006; Daddi
et al. 2000).
Counts in 7C 1751+6908 are consistent, if anything slightly
lower, than the average of E-CDFS. The counts of pBzK*
and sBzK galaxies around 7C 1756+6520 on
the contrary fall way beyond the average density in E-CDFS, near the
end of the tail of the distribution with only 0.26% of the cells having
similar densities, confirming the result that the HzRG is found in an
exceptionally overdense region.
3.4 Number counts
We derive the Ks-band number counts in 0.5 mag bins
for pBzK, pBzK* and sBzK
galaxies in
our two fields (Fig. 7).
We adopt Poissonian
errors for the counts and use the Gehrels
(1986) small numbers approximation for Poisson distributions.
We overplot the findings of Kong et al. (2006; K06 hereafter)
as a dotted line for comparison (see also Lane
et al. 2007; Imai
et al. 2008; Hartley
et al. 2008).
The number counts become incomplete at
when we start reaching the
completeness limit of our z-band.
The number counts of pBzK and sBzK
galaxies are in good agreement with Kong
et al. (2006). We find the number of sBzK
galaxies increasing steeply with decreasing magnitude, with the slope
for the 7C 1756+6520 field similar to K06.
7C 1751+6809, however, shows a small excess ()
of sBzK galaxies at bright Ks
magnitudes (
).
The slope of the number counts for pBzK galaxies is
similar for both of our radio galaxy fields and Kong
et al. (2006). A small excess of Ks-bright
pBzK galaxies is suggested in both fields (
). Such
excesses of Ks-bright galaxies have also been
noticed around other HzRGs (Kodama
et al. 2007). If these Ks-bright
sources were associated with the HzRGs, they would be very massive (
)
and would represent the massive, evolved galaxy population of a young
galaxy cluster around the HzRG. However, the number of sources
considered here is too small to reach any firm conclusion since we
detect only five pBzK galaxies with
.
Previous work (K06; Lane
et al. 2007; Hartley
et al. 2008)
has shown that the pBzK number counts show a turn
over at K > 21 with the counts slope
flattening at
fainter sources. We also strongly suspect this flattening in our counts
although our BzK selection rapidly becomes
incomplete at
.
A possible explanation for this turn-over is that pBzK
galaxies are selected in a small redshift range and consist of very
massive, passively evolving galaxies. Due to downsizing, their number
decrease at lower luminosities (Hartley
et al. 2008). The slope of the counts and the range
of Ks magnitudes sampled by the pBzK*
galaxies are also consistent with the pBzK galaxies,
suggesting that our extended selection criteria is also likely to be
selecting galaxies in the same redshift range.
![]() |
Figure 9:
Radial density profile of BzK selected galaxies
around 7C1756+6520 ( upper panels) and
7C 1751+6809 ( lower panels) for pBzK*
galaxies ( left panels) and sBzK
galaxies ( right panels). The full field density is
shown by the horizontal dashed lines. The profiles and surface
densities were derived from the entire sample of candidates. The values
obtained are therefore
higher than in Table 1
where the study was restricted to the completeness limit. The error
bars indicate the |
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4 Properties of candidate massive cluster members
4.1 Spatial distribution
![]() |
Figure 10:
Color-magnitude diagram (J-Ks vs.
Ks) of the regions surrounding the HzRGs
(within 3'). The pBzK* and sBzK
galaxies are plotted as red circles and blue triangles respectively. sBzK
galaxies not detected
in J are shown as blue arrows. Also plotted are all
sources in this same region detected in the three BzK
bands (black dots). The radio galaxies are shown as red stars. The
dotted lines represent the |
Open with DEXTER |








The sBzK galaxies also have an inhomogenous
distribution though it is less well defined than the pBzK*
galaxies. In particular, 7C 1756+6520 has nine sBzK
galaxies along the same elongated structure near the HzRG. One sBzK
galaxy is also found near the line of sight of the HzRG (at
,
Fig. 12).
The sBzK galaxies in the 7C 1751+6809 field
show an excess near the center of the field with an elongation in the
direction NW-SE with no obvious correlation with the pBzK*
spatial distribution. This overdensity was not seen with the density
counts in Table 2,
most probably due to the fact that the HzRG is at the ``edge'' of the
elongated structure of sBzK galaxies. If associated
with the HzRG, this structure would have a
4 Mpc extent.
Figure 9
presents the radial distribution of pBzK* and sBzK
galaxies around
both HzRGs i.e., the number of candidates found per radius bin (binsize
)
divided by
the corresponding ring area. The large error bars are due to the small
number of sources used
to derive the radial profiles, e.g., only 5 pBzK*
and 1 sBzK galaxies are found
within
of 7C 1756+6520. The distribution of candidates near
7C 1756+6520 forms an elongated structure, not centered around
the HzRG.
The radial profile in Fig. 9
is therefore a lower limit to the true concentration of BzKaround
the HzRG as it does not fully reflect the complex spatial distribution
of the sources. However, we note that a clear peak of pBzK*
galaxies is seen near the HzRG. The pBzK* density
decreases with radius and asymptotes to the full field density (red
dashed line)
at
from the radio galaxy.
Variations are also observed in the profile of
the sBzK galaxies
with a deficit of sources near the HzRG (<
)
and a ``bump'' in the profile between
and
,
suggestive of some segregation in the properties
of the galaxies in the large scale structure. We note however that the
significance of those variations is less that
.
As seen previously, no significant variation of the pBzK*
density is seen around 7C 1751+6809 but a small overdensity of
sBzK is observed within
of the HzRG (
significant though).
4.2 Color-magnitude diagram
Color-magnitude diagrams (CMDs) are an efficient method to study the
formation and evolution of galaxies. At z <
1, galaxy cluster cores are dominated by massive, passively-evolving
elliptical galaxies that trace a clear red sequence on the
color-magnitude diagram. In the last decade, studies have shown that
this red sequence of early-type galaxies is also found in galaxy
clusters out to
(e.g. Stanford
et al. 2006; Mei
et al. 2006; Lidman
et al. 2008; Tanaka
et al. 2007).
Recent work at even higher redshifts have studied the evolved galaxy
population in
galaxy clusters and conclude that the red sequence may appear between z
= 3 and 2 (Zirm
et al. 2008; Kodama
et al. 2007).
We have investigated the CMD of the sources in the region surrounding
the HzRGs. Their CMDs are shown in Fig. 10. Sources
within 3'
of the HzRGs and with a
detection in all BzK bands are plotted as black
dots. The size of the studied region was chosen as a compromise between
selecting sources close to the HzRG and including the majority of the
candidates in the apparent central overdensity. We note that the region
of the CMD at faint Ks magnitude starts to be empty
well before the magnitude limit of our Ks-band data
due to the non detection of faint Ks sources in the
optical bands. pBzK* and sBzK
galaxies within 3' (
1.5 Mpc
at z=1.5) are plotted as red points and blue
triangles, respectively. All pBzK* galaxies found
near the HzRGs have a >
detection in the J-band; sBzK
galaxies with lower limits in J are marked as blue
arrows. The two pBzK* galaxies found near both HzRGs
and the sBzK galaxy found near 7C 1756+6520
are marked as squares. We overplot models of the expected location of
the red sequence at z=1.5, i.e., the
predicted J-K color of a
passively evolving galaxy with different formation redshifts (
,
4, 5; provided by Kodama). The models reproduce the red sequence of
passively evolving galaxies in the Coma cluster at z=0
and include a metallicity-magnitude dependance which causes the red
sequence slope (Kodama
et al. 1998).
![]() |
Figure 11:
Mid-IR color-color diagram for 7C 1756+6520 ( top)
and 7C 1751+6809 ( bottom).
All sources with a |
Open with DEXTER |
The pBzK* galaxies in the inner
region around 7C 1756+6520 have colors consistent with
passively evolving galaxies with
in contrast to the pBzK* galaxies around
7C 1751+6809 which have bluer J-Ks
colors. Some elliptical candidates have slightly redder colors (
)
and may be background objects since the BzK
criteria is designed to select objects at
1.4 < z < 2.5. Two of the pBzK*
and three of the sBzK galaxies have
and would be classified as DRGs, i.e., they are likely to be
either passive elliptical or dusty star-forming galaxies at z
> 2.
Recent observations of some high redshift galaxy clusters have
shown a deficit of red galaxies at the faint end of the red sequence
compared to local clusters (Tanaka
et al. 2005,2007; De Lucia
et al. 2007; Kajisawa
et al. 2000).
It has been suggested that the red sequence appears at bright
magnitudes and progressively extends to fainter magnitudes with time. Tanaka
et al. (2007)
studied a possible large-scale structure around a galaxy cluster at z
= 1.24 and found that a deficit of faint red galaxies is noted in the
clumps surrounding the central cluster but not in the CMD of the
cluster itself, suggesting that the build-up of the red sequence is
dependent on environment, progressing more rapidly in higher density
environments. Considering the potential cluster around
7C 1756+6520, we note a clear deficit of Ks-faint
pBzK* galaxies. No pBzK* galaxy
is found with
near the HzRG. At these faint Ks magnitudes, we
surely reach the combined incompleteness of our z
and Ks bands data. But, as described in
Sect. 3.2, we are more than 60% complete at our magnitude
limits. For example, 29 pBzK* galaxies with
are found in the full field and sBzK galaxies are
found with
within 3' of the HzRG. We therefore conclude
that the truncation at faint magnitudes is real. This would imply that
this is another example of downsizing (Cowie
et al. 1996); i.e., the more massive cluster members
stopped their star-formation
earlier than the less massive cluster members. A similar study of the
CMD of red galaxies in the field of the X-ray galaxy cluster
XMMUJ2235.3-2557 at z=1.39 is presented in Lidman
et al. (2008).
They do not observe evidence of a truncation of the red sequence at
fainter magnitudes, suggesting that
they are looking at a richer or more evolved system.
The scatter of the pBzK* galaxies relative to the
red sequence model at
(
)
is
(
)
magnitudes for non-DRG galaxies. This scatter is large and
most probably inflated by non-cluster members. Studies of the intrinsic
scatter of the red sequence in galaxy clusters at
1.2 < z < 1.5 have however shown that
the scatter in J-K can be up
to
0.06
(Lidman
et al. 2008,2004).
We stress that the pBzK* galaxies selected in this work are only candidate cluster members and that spectroscopic follow-up will be necessary to confirm their physical association to the HzRGs.
5 AGN candidates
Recent studies suggest that AGN companions are often found around radio galaxies. Croft et al. (2005) spectroscopically confirmed three QSOs in the surroundings of PKS 1138-262 at z=2.16 and suggested that the QSOs were triggered by the protocluster formation (see also Pentericci et al. 2000). Venemans et al. (2007) also detected QSOs near radio-galaxies at z > 3. Recently, Galametz et al. (2009a) studied the AGN population in a large sample of galaxy clusters at z < 1.5 and found an excess of AGN within 0.5 Mpc of the cluster centers, with the number of AGN in clusters increasing with redshift (see also Eastman et al. 2007). Powerful AGN provide an alternative way to look for relatively massive host galaxies in a complementary technique to the near-IR color selection.
Stern
et al. (2005)
presents a robust technique for identifying active galaxies from
mid-infrared color criteria (see also Lacy
et al. 2004). While the continuum emission of
stellar populations peaks at approximately m, the continuum of AGN is
dominated by a power law throughout the mid-infrared. Stern et al.
(2005)
adopt the following (Vega system) criteria
to isolate AGN from other sources:
Since
the criterion is designed to identify power-law spectra, they do not
preferentially
select AGN in any specific redshift range.
We apply this selection criteria to all sources with a
detection in all four IRAC bands. The coordinates of the selected AGN
for 7C 1756+6520 (12 candidates) and 7C 1751+6809
(5 candidates) are given in Table 3 and
Table 4,
respectively. Figure 11
shows their distributions in the [3.6]-[4.5] vs [5.8]-[8.0] color-color
diagram.
We note that although neither HzRG is detected at a
level in the
m-band,
their IRAC magnitudes and position in the IRAC color-color diagram are
presented in the tables and in Fig. 11. Both are
undeniably
classified as AGN by the Stern
et al. (2005) criterion.
As a comparison field, we use the IRAC Shallow Survey (ISS; Eisenhardt
et al. 2004),
which includes four IRAC bands and covers 8 square degrees in the
Boötes field with at least 90 s exposure time per position.
2262 sources in ISS are found in the Stern
et al. (2005) AGN selection wedge, where we require
a
detections in all four IRAC bands (Galametz
et al. 2009a).
The
m
band is the least sensitive with a
limiting depth of 15.9 (Vega, in an
aperture-corrected
diameter aperture; equivalent to
Jy). Whereas we would expect
three to four AGN candidates in the HzRG fields, we find 8 AGN
candidates near 7C 1756+6520 and four near
7C 1751+6809 at the depth of ISS. We therefore observe an
overdensity of AGN candidates in the field of 7C 1756+6520 by
a factor of two compared to the 7C 1751+6809 and ISS fields.
One AGN candidate is found only
offset from 7C 1756+6520 (Fig. 12,
Sect. 6)
and two additional candidates are found within
of
the HzRG. However, the 12 AGN candidates do not show any particular
spatial distribution as was seen for both the pBzK*
and sBzK galaxies (see Sect. 4.2). No AGN
candidate
is found within
of 7C 1751+6809.
![]() |
Figure 12:
7C 1756+6520 and its immediate surroundings in our Palomar/LFC
B and z-bands,
CFHT/WIRCAM J and Ks-bands, and
Spitzer/IRAC |
Open with DEXTER |
6 Candidate close companions to 7C 1756+6520
An elliptical, a star-forming and an AGN candidate are found near the
line of sight
to 7C 1756+6520 (within
),
suggestive of several close
companions. Figure 12
shows the immediate surroundings of 7C 1756+6520 in our
imaging bands; arrows indicate the pBzK* galaxies, sBzK
galaxies and the AGN candidate. Using the density of BzK
galaxies found in the full field, we find that the probability of
finding a pBzK* galaxy within
of the HzRG is
0.44%,
and the probability of finding a sBzK galaxy is
0.54%. At
the depth of our IRAC data, the probability of finding an AGN candidate
in the same area is
0.57%.
The probability of finding the three candidates in this small area
around the HzRG is therefore extremely small,
strongly suggesting that these candidates are associated with the HzRG
and
form a very unique and diverse system of bound galaxies.
7 Conclusions
We study of the surroundings of two radio galaxies at
using deep
multiwavelength imaging. We select candidate cluster members using
color selection techniques designed to select galaxies at the redshift
of the targeted HzRG. This technique has been proven to identify
clusters and proto-clusters at high redshift (z
>
2; Tanaka
et al. 2007; Kajisawa
et al. 2006).
An excess of candidate passive elliptical candidates is found in the
field of one of our two targets, 7C 1756+6520 by a factor of
compared to control fields. A study of the counts-in-cells fluctuations
in our larger control field shows that the probability to find such an
overdensity in the field is very low (0.26%). These results may be
compared to previous studies that have been made at similar or higher
redshifts. The Best
et al.
(2003) study of the environments of six radio-loud AGN at
finds an excess by a factor of 1.5 to 4 of EROs within radial distances
of
1 Mpc
of the AGN. Similarly, Kodama
et al. (2007) select passive evolving and star
forming cluster member candidates in the surroundings of four HzRGs
with 2 < z < 3 applying color cuts in
JHKs and found excesses by a factor of two to three
compared to the field. Clusters were already suspected around those
HzRGs in previous studies that were concentrated on overdensities of
narrow-band (H
,
Ly
)
emitters also by a factor of two to five larger than in the field (Venemans
et al. 2005,2007; Kurk
et al. 2004a).
Looking at narrow-band emitters has been very efficient at finding
overdensities around HzRGs. However, such clusters members, dominated
by young stellar populations, are likely not the most massive members
of the galaxy clusters. Indeed, recent studies show that Ly
emitters have rather small stellar masses. Finkelstein
et al. (2007)
found masses ranging from
to
for a sample of 98 Ly
emitters at
.
Similar masses were deduced from Ly
emitters in Gawiser
et al. (2007) who found stellar masses of
for lower redshift objects (
). Looking at the properties
of Ly
emitters, members of a protocluster at z = 4.1, Overzier
et al. (2008)
derived a mean stellar mass of
based on stacked Ks-band images, indicating that Ly
emitters in the field and in protoclusters at high redshift have
similar masses. Kurk
et al.
(2004b) used near infrared magnitudes to derive the stellar
masses of H
emitters found in the overdensity surrounding PKS 1138-262, a
well known protocluster at z = 2.16, and
found that H
emitters are more massive than Ly
emitters, with a stellar mass
.
The total stellar mass derived from both Ly
and H
emitters around PKS 1138-262 (40 sources) is
(Kurk et al.
2004b).
The mass function of galaxy clusters is in fact dominated by the
evolved galaxy population, known to be rarer but much more massive than
the narrow-band emitters (e.g., for
,
;
Kodama
et al. 2007).
If at
,
the two objects with
found within
o2f 7C 1756+6520 would each have a stellar mass of
and would therefore already have a mass equivalent to all the
narrow-band emitters found near PKS 1138-262.
It is therefore essential to search for this population of red
elliptical galaxies to fully understand
the earliest phases of cluster formation.
Our study makes use of wide-field optical and near-infrared cameras and permits the investigation of the spatial distribution of potential cluster members over a large area around the HzRG. Indeed, the small field of view of the previous generation of near-infrared instruments limited the study of large-scale structures, clusters and proto-clusters. Recently, Tanaka et al. (2007) presented a study of a large-scale structure around a galaxy cluster at z=1.24 with a possible large (20 Mpc) filamentary structure formed by the main cluster and four possible associated clumps of red galaxies, illustrating the necessity to look at galaxy clusters on larger scales than the cluster itself. The 7C 1756+6520 field presents several overdensities of red objects separated by several arcmin, as well as one nearby the HzRG. However, spectroscopic confirmation of these extended structures being associated and at high redshift is challenging due of the required large field of view on a multi-object spectrograph, and the high redshift which places the main spectral features (emission lines for star-forming and breaks for elliptical galaxies) out of the optical bands. This will hopefully be achieved with the new generation of multi-object, near-infrared spectrographs (e.g., MOIRCS on Subaru).
AcknowledgementsWe are very grateful to S. Adam Stanford for useful discussions and Tadayuki Kodama for having provided the models of red sequences presented in this paper. We thank Brigitte Rocca-Volmerange for her support of this project. We would also like to thank Andrea Grazian (and the GOODS-MUSIC team) and Ryan Quadri (and the MUSYC survey team) for useful emails exchanges on their online catalogs. This work is based in part on data products produced at the TERAPIX data center located at the Institut d'Astrophysique de Paris and generated from observations obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. It is also based on observations obtained at the Hale 200 inch telescope at Palomar Observatory and on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA.
References
- Abraham, R. G., Glazebrook, K., McCarthy, P. J., et al. 2004, AJ, 127, 2455 [CrossRef] [NASA ADS]
- Bertin, E., & Arnouts, S. 1996, A&AS, 117, 393 [EDP Sciences] [CrossRef] [NASA ADS]
- Best, P. N., Lehnert, M. D., Miley, G. K., & Röttgering, H. J. A. 2003, MNRAS, 343, 1 [CrossRef] [NASA ADS]
- Borgani, S., Rosati, P., Tozzi, P., et al. 2001, ApJ, 561, 13 [CrossRef] [NASA ADS]
- Bruzual, G., & Charlot, S. 2003, MNRAS, 344, 1000 [CrossRef] [NASA ADS]
- Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, ApJ, 345, 245 [CrossRef] [NASA ADS]
- Carilli, C. L., Harris, D. E., Pentericci, L., et al. 2002, ApJ, 567, 781 [CrossRef] [NASA ADS]
- Cimatti, A., Daddi, E., Mignoli, M., et al. 2002, A&A, 381, L68 [EDP Sciences] [CrossRef] [NASA ADS]
- Cimatti, A., Auvergne, M., Baglin, A., et al. 2008, A&A, 482, 21 [EDP Sciences] [CrossRef] [NASA ADS]
- Cool, R. J. 2007, ApJS, 169, 21 [CrossRef] [NASA ADS]
- Cowie, L. L., Songaila, A., Hu, E. M., & Cohen, J. G. 1996, AJ, 112, 839 [CrossRef] [NASA ADS]
- Croft, S., Kurk, J., van Breugel, W., et al. 2005, AJ, 130, 867 [CrossRef] [NASA ADS]
- Daddi, E., Cimatti, A., Pozzetti, L., et al. 2000, A&A, 361, 535 [NASA ADS]
- Daddi, E., Cimatti, A., Renzini, A., et al. 2004, ApJ, 617, 746 [CrossRef] [NASA ADS]
- De Lucia, G., Poggianti, B. M., Aragón-Salamanca, A., et al. 2007, MNRAS, 374, 809 [CrossRef] [NASA ADS]
- Eastman, J., Martini, P., Sivakoff, G., et al. 2007, ApJ, 664, L9 [CrossRef] [NASA ADS]
- Eisenhardt, P. R., Stern, D., Brodwin, M., et al. 2004, ApJS, 154, 48 [CrossRef] [NASA ADS]
- Eke, V. R., Cole, S., Frenk, C. S., & Patrick Henry, J. 1998, MNRAS, 298, 1145 [CrossRef] [NASA ADS]
- Elston, R. J., Gonzalez, A. H., McKenzie, E., et al. 2006, ApJ, 639, 816 [CrossRef] [NASA ADS]
- Fazio, G. G., Hora, J. L., Allen, L. E., et al. 2004, ApJS, 154, 10 [CrossRef] [NASA ADS]
- Finkelstein, S. L., Rhoads, J. E., Malhotra, S., Pirzkal, N., & Wang, J. 2007, ApJ, 660, 1023 [CrossRef] [NASA ADS]
- Finlator, K., Ivezic, Zdeljko; F. X., et al. 2000, AJ, 120, 2615 [CrossRef] [NASA ADS]
- Fioc, M., & Rocca-Volmerange, B. 1997, A&A, 326, 950 [NASA ADS]
- Franx, M., Labbé, I., Rudnick, G., et al. 2003, ApJ, 587, L79 [CrossRef] [NASA ADS]
- Galametz, A., Stern, D., Eisenhardt, P. R. M., et al. 2009a, ApJ, 694, 1309 [CrossRef] [NASA ADS]
- Gawiser, E., van Dokkum, P. G., Herrera, D., et al. 2006, ApJS, 162, 1 [CrossRef] [NASA ADS]
- Gawiser, E., Francke, H., Lai, K., et al. 2007, ApJ, 671, 278 [CrossRef] [NASA ADS]
- Gehrels, N. 1986, ApJ, 303, 336 [CrossRef] [NASA ADS]
- Grazian, A., Fontana, A., Moscardini, L., et al. 2006a, A&A, 453, 507 [EDP Sciences] [CrossRef] [NASA ADS]
- Grazian, A., Fontana, A., de Santis, C., et al. 2006b, A&A, 449, 951 [EDP Sciences] [CrossRef] [NASA ADS]
- Grazian, A., Salimbeni, S., Pentericci, L., et al. 2007, A&A, 465, 393 [EDP Sciences] [CrossRef] [NASA ADS]
- Hartley, W. G., Lane, K. P., Almaini, O., et al. 2008, MNRAS, 391, 1301 [CrossRef] [NASA ADS]
- Imai, K., Pearson, C. P., Matsuhara, H., et al. 2008, ApJ, 683, 45 [CrossRef] [NASA ADS]
- Kajisawa, M., Yamada, T., Tanaka, I., et al. 2000, PASJ, 52, 61 [NASA ADS]
- Kajisawa, M., Kodama, T., Tanaka, I., Yamada, T., & Bower, R. 2006, MNRAS, 371, 577 [CrossRef] [NASA ADS]
- Kodama, T., Arimoto, N., Barger, A. J., & Arag'on-Salamanca, A. 1998, A&A, 334, 99 [NASA ADS]
- Kodama, T., Tanaka, I., Kajisawa, M., et al. 2007, MNRAS, 377, 1717 [CrossRef] [NASA ADS]
- Kong, X., Daddi, E., Arimoto, N., et al. 2006, ApJ, 638, 72 [CrossRef] [NASA ADS]
- Kurk, J. D., Pentericci, L., Overzier, R. A., Röttgering, H. J. A., & Miley, G. K. 2004a, A&A, 428, 817 [EDP Sciences] [CrossRef] [NASA ADS]
- Kurk, J. D., Pentericci, L., Röttgering, H. J. A., & Miley, G. K. 2004b, A&A, 428, 793 [EDP Sciences] [CrossRef] [NASA ADS]
- Kurk, J. D., Cimatti, A., Daddi, E., et al. 2008, in Infrared Diagnostics of Galaxy Evolution, ASP Conf. Ser., 381, 303
- Lacy, M., Rawlings, S., & Warner, P. J. 1992, MNRAS, 256, 404 [NASA ADS]
- Lacy, M., Rawlings, S., Hill, G. J., et al. 1999, MNRAS, 308, 1096 [CrossRef] [NASA ADS]
- Lacy, M., Storrie-Lombardi, L. J., Sajina, A., et al. 2004, ApJS, 154, 166 [CrossRef] [NASA ADS]
- Lacy, M., Wilson, G., Masci, F., et al. 2005, ApJS, 161, 41 [CrossRef] [NASA ADS]
- Landolt, A. U. 1992, AJ, 104, 340 [CrossRef] [NASA ADS]
- Lane, K. P., Almaini, O., Foucaud, S., et al. 2007, MNRAS, 379, L25 [NASA ADS]
- Lidman, C., Rosati, P., Demarco, R., et al. 2004, A&A, 416, 829 [EDP Sciences] [CrossRef] [NASA ADS]
- Lidman, C., Rosati, P., Tanaka, M., et al. 2008, A&A, 489, 981 [EDP Sciences] [CrossRef] [NASA ADS]
- Maihara, T., Iwamuro, F., Tanabe, H., et al. 2001, PASJ, 53, 25 [NASA ADS]
- Makovoz, D., & Khan, I. 2005, in Astronomical Data Analysis Software and Systems XIV, ed. P. Shopbell, M. Britton, & R. Ebert, ASP Conf. Ser., 347, 81
- Marmo, C. 2007, in Astronomical Data Analysis Software and Systems XVI, ed. R. A. Shaw, F. Hill, & D. J. Bell, ASP Conf. Ser., 376, 285
- Matthews, T. A., Morgan, W. W., & Schmidt, M. 1964, ApJ, 140, 35 [CrossRef] [NASA ADS]
- Mei, S., Holden, B. P.,; Blakeslee, J. P., et al. 2006, ApJ, 644, 759 [CrossRef] [NASA ADS]
- Metcalfe, N., Shanks, T., Fong, R., & Jones, L. R. 1991, MNRAS, 249, 498 [NASA ADS]
- Metcalfe, N., Shanks, T., Fong, R., & Roche, N. 1995, MNRAS, 273, 257 [NASA ADS]
- Miley, G. K., Overzier, R. A., Tsvetanov, Z. I., et al. 2004, Nature, 427, 47 [CrossRef] [NASA ADS]
- Mobasher, B., Idzi, R., Benítez, N., et al. 2004, ApJ, 600, L167 [CrossRef] [NASA ADS]
- Monet, D. G., Levine, S. E., Canzian, B., et al. 2003, AJ, 125, 984 [CrossRef] [NASA ADS]
- Mullis, C. R., Rosati, P., Lamer, G., et al. 2005, ApJ, 623, L85 [CrossRef] [NASA ADS]
- Overzier, R. A., Bouwens, R. J., Cross, N. J. G., et al. 2008, ApJ, 673, 143 [CrossRef] [NASA ADS]
- Pentericci, L., Kurk, J. D., Röttgering, H. J. A., et al. 2000, A&A, 361, L25 [NASA ADS]
- Puget, P., et al. 2004, in Ground-based Instrumentation for Astronomy, ed. A. F. M. Moorwood, & I. Masanori, Proc. SPIE, 5492, 978
- Quadri, R., Marchesini, D., van Dokkum, P., et al. 2007, AJ, 134, 1103 [CrossRef] [NASA ADS]
- Reddy, N. A., Steidel, C. C., Fadda, D., et al. 2006, ApJ, 644, 792 [CrossRef] [NASA ADS]
- Rettura, A., et al. 2008, ApJ, 806
- Santini, P., et al. 2009, ArXiv e-prints
- Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, 500, 525 [CrossRef] [NASA ADS]
- Seymour, N., Stern, D., De Breuck, C., et al. 2007, ApJS, 171, 353 [CrossRef] [NASA ADS]
- Simcoe, R. A., Metzger, M. R., Small, T. A., & Araya, G. 2000, in BAAS, 32, 758
- Skrutskie, M. F., et al. 1997, in The Impact of Large Scale Near-IR Sky Surveys, ed. F. Garzon, N. Epchtein, A. Omont, B. Burton, & P. Persi, Ap&SS Library, 210, 25
- Stanford, S. A., Romer, A. K., Sabirli, K., et al. 2006, ApJ, 646, L13 [CrossRef] [NASA ADS]
- Stern, D., Holden, B., Stanford, S. A., & Spinrad, H. 2003, AJ, 125, 2759 [CrossRef] [NASA ADS]
- Stern, D., Eisenhardt, P., Gorjian, V., et al. 2005, ApJ, 631, 163 [CrossRef] [NASA ADS]
- Stern, D., Jimenez, R., Verde, L., Kamionkowski, M., & Stanford, S. A. 2009 [arXiv:0907.3149]
- Tanaka, M., Kodama, T., Arimoto, N., et al. 2005, MNRAS, 362, 268 [CrossRef] [NASA ADS]
- Tanaka, M., Kodama, T., Kajisawa, M., et al. 2007, MNRAS, 377, 1206 [CrossRef] [NASA ADS]
- Teplitz, H. I., McLean, I. S., & Malkan, M. A. 1999, ApJ, 520, 469 [CrossRef] [NASA ADS]
- Venemans, B. P., Röttgering, H. J. A., Miley, G. K., et al. 2005, A&A, 431, 793 [EDP Sciences] [CrossRef] [NASA ADS]
- Venemans, B. P., Röttgering, H. J. A., Miley, G. K., et al. 2007, A&A, 461, 823 [EDP Sciences] [CrossRef] [NASA ADS]
- Williams, R. E., Blacker, B., Dickinson, M., et al. 1996, AJ, 112, 1335 [CrossRef] [NASA ADS]
- York, D. G., Adelman, J., Anderson, J. E., Jr., et al. 2000, AJ, 120, 1579 [CrossRef] [NASA ADS]
- Zirm, A. W., Stanford, S. A., Postman, M., et al. 2008, ApJ, 680, 224 [CrossRef] [NASA ADS]
Online Material
Table 2: Surface densities of BzK galaxies (to the completeness limits; degrees-2).
Table 3: AGN candidates in 7C 1756+6520 field.
Table 4: AGN candidates in 7C 1751+6809 field.
Table 5: pBzK* galaxies in 7C 1756+6520 field.
Table 6: pBzK* galaxies in 7C 1751+6809 field.
Footnotes
- ... 1.5
- Tables 2-6 are only available in electronic form at http://www.aanda.org
- ... 1.48
- A new spectrum obtained with Keck/Deimos in September 2009 revealed a new redshift z=1.416 for the radio galaxy 7C1756+6520 (based on [NeV]3426, [OII]3727, and [NeIII]3869). This is different from the tentative z=1.48 reported by Lacy et al. (1999), but does not affect the colour selections or conclusions in this paper.
- ...
collaboration
- See http://www.sdss.org/DR2/algorithms/fluxcal.html.
- ...
team
- http://terapix.iap.fr
- ... 23.4
- The final catalogs and images are available at http://archive.noao.edu/nsa/zbootes.html.
- ... 2)
- The GDDS catalog is publicly available at http://lcirs.ociw.edu/public/GDDSSummary-dist.txt. Targeted magnitudes are in the Vega system. We convert from Vega to the AB photometric system using the corrections adopted earlier in this paper.
- ... dataset
- The full catalog, including photometric redshifts, is publicly available at http://lbc.mporzio.astro.it/goods/goods.php.
- ...
website
- http://www.astro.yale.edu/MUSYC/
- ... criteria
- We use the following conversions between the Vega and AB
photometric systems:
,
,
and
.
All Tables
Table 1: Observations.
Table 2: Surface densities of BzK galaxies (to the completeness limits; degrees-2).
Table 3: AGN candidates in 7C 1756+6520 field.
Table 4: AGN candidates in 7C 1751+6809 field.
Table 5: pBzK* galaxies in 7C 1756+6520 field.
Table 6: pBzK* galaxies in 7C 1751+6809 field.
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