We construct a galaxy groups catalogue from the public 100K data release of the 2dF galaxy redshift survey. The group identification is carried out using a slightly modified version of the group ...finding algorithm developed by Huchra & Geller. Several tests using mock catalogues allow us to find the optimal conditions to increase the reliability of the final group sample. A minimum number of 4 members, an outer number density enhancement of 80 and a linking radial cutoff of \(200 km sec^{-1}\), are the best obtained values from the analysis. Using these parameters, approximately 90% of groups identified in real space have a redshift space counterpart. On the other hand the level of contamination in redshift space reaches to 30 % including a \(\sim 6%\) of artificial groups and \(\sim 24%\) of groups associated with binaries or triplets in real space. The final sample comprise 2209 galaxy groups covering the sky region described by Colless et al. spanning over the redshift range of \(0.003 \leq z \leq 0.25\) with a mean redshift of 0.1.
Fossil systems are defined to be X-ray bright galaxy groups with a 2-magnitude difference between their two brightest galaxies within half the projected virial radius,and represent an interesting ...extreme of the population of galaxy agglomerations.However,the physical conditions and processes leading to their formation are still poorly constrained.We compare the outskirts of fossil systems with that of normal groups to understand whether environmental conditions play a significant role in their formation.We study galaxy groups in both,numerical simulations and observations.We use a variety of statistical tools including the spatial cross-correlation function and the local density parameter \Delta_5 to probe differences in the density and structure of the environments of normal and fossil systems in the Millennium simulation.We find that the number density of galaxies surrounding fossil systems evolves from greater than that observed around normal systems at z=0.69, to lower than the normal systems by z=0.Both fossil and normal systems exhibit an increment in their otherwise radially declining local density measure (\Delta_5) at distances of order 2.5r_{vir} from the system centre.We show that this increment is more noticeable for fossil systems than normal systems and demonstrate that this difference is linked to the earlier formation epoch of fossil groups.Despite the importance of the assembly time, we show that the environment is different for fossil and non-fossil systems with similar masses and formation times along their evolution.We also confirm that the physical characteristics identified in the Millennium simulation can also be detected in SDSS observations.Our results confirm the commonly held belief that fossil systems assembled earlier than normal systems but also show that the surroundings of fossil groups could be responsible for the formation of their large magnitude gap.
Astrophys.J.650:137-147,2006 Using galaxy groups identified in the Fourth Data Release of the Sloan
Digital Sky Survey (SDSS), we compute the luminosity function for several
subsamples of galaxies in ...groups. In all cases, the luminosity functions are
well described by Schechter functions, down to the faintest magnitudes we
probe, $M_{\rb}-5\log(h)\sim-16$. For the general luminosity function of
galaxies in groups in the five SDSS bands, we observe that the characteristic
magnitude is brighter in $\sim 0.5$ magnitudes compared to those obtained for
field galaxies by Blanton et al.. Even when the observed faint end slope is
steeper in galaxy groups, it is statistically comparable with the field value.
We analyze the dependence of the galaxy luminosity function with system masses
finding two clear trends: a continuous brightening of the characteristic
magnitude and a steepening of the faint end slope as mass increases. The
results in $\gb$, $\rb$, $\ib$ and $\zb$ bands show the same behavior. Using
the $u-r$ color to split the galaxy sample into red and blue galaxies, we show
that the changes observed as a function of the system mass are mainly seen in
the red, passively evolving, galaxy population, while the luminosities of blue
galaxies remain almost unchanged with mass. Finally, we observe that groups
having an important luminosity difference between the two brightest galaxies of
a system show a steeper faint end slope than the other groups. Our results can
be interpreted in terms of galaxy mergers as the main driving force behind
galaxy evolution in groups.
Astrophys.J. 629 (2005) 158-171 We have analysed the distribution of galaxies in groups identified in the
largest redshift surveys at the present: the final release of the 2dF Galaxy
Redshift Survey ...and the first release of the Sloan Digital Sky Survey. Our work
comprises the study of the galaxy density profiles and the fraction of galaxies
per spectral type as a function of the group-centric distance. We have
calculated the projected galaxy density profiles of galaxy groups using
composite samples in order to increase the statistical significance of the
results. Special cares have been taken in order to avoid possible biases in the
group identification and the construction of the projected galaxy density
profile estimator. The results show that the projected galaxy density profiles
obtained for both redshift surveys are in agreement with a projected Navarro,
Frenk & White predictions in the range $0.15< r/r_{200}
< 1$, whereas a good fit for the measured profiles in the whole range of
$r/r_{200}$ is given by a projected King profile. We have adopted a generalized
King profile to fit the measured projected density profiles per spectral type.
In order to infer the 3-D galaxy density profiles, we deproject the 2-D density
profiles using a deprojection method similar to the developed by Allen &
Fabian. From 2-D and 3-D galaxy density profiles we have estimated the
corresponding galaxy fractions per spectral type. The 2-D fraction of galaxies
computed using the projected profiles show a similar segregation of galaxy
spectral types as the obtained by Dom\'{\i}nguez et al. for groups in the early
data release of the 2dF Galaxy Redshift Survey. As expected, the trends
obtained for the 3-D galaxy fractions show steeper slopes than the observed in
the 2-D fractions.
Mon.Not.Roy.Astron.Soc. 344 (2003) 247 We use the 2dF Galaxy Group Catalogue constructed by Merch\'an & Zandivarez
to study the large scale structure of the Universe traced by galaxy groups. We
...concentrate on the computation of the power spectrum and the two point
correlation function. The resulting group power spectrum shows a similar shape
to the galaxy power spectrum obtained from the 2dF Galaxy Redshift Survey by
Percival et al., but with a higher amplitude quantified by a relative bias in
redshift space of $b_s(k) \sim 1.5$ . The group two point correlation function
for the total sample is well described by a power law with correlation length
$s_0=8.9 \pm 0.3 \mpc$ and slope $\gamma=-1.6 \pm 0.1$ on scales $s < 20 \mpc$.
In order to study the dependence of the clustering properties on group mass we
split the catalogue in four subsamples defined by different ranges of group
virial masses. These computations allow a fair estimate of the relation
described by the correlation length $s_0$ and the mean intergroup separation
$d_c$ for galaxy systems of low mass. We also extend our study to the redshift
space distortions of galaxy groups, where we find that the anisotropies in the
clustering pattern of the 2dF group catalogue are consistent with gravitational
instability, with a flattening of the redshift-space correlation function
contours in the direction of the line of sight.
Using galaxy groups identified in the Fourth Data Release of the Sloan Digital Sky Survey (SDSS), we compute the luminosity function for several subsamples of galaxies in groups. In all cases, the ...luminosity functions are well described by Schechter functions, down to the faintest magnitudes we probe, \(M_{\rb}-5\log(h)\sim-16\). For the general luminosity function of galaxies in groups in the five SDSS bands, we observe that the characteristic magnitude is brighter in \(\sim 0.5\) magnitudes compared to those obtained for field galaxies by Blanton et al.. Even when the observed faint end slope is steeper in galaxy groups, it is statistically comparable with the field value. We analyze the dependence of the galaxy luminosity function with system masses finding two clear trends: a continuous brightening of the characteristic magnitude and a steepening of the faint end slope as mass increases. The results in \(\gb\), \(\rb\), \(\ib\) and \(\zb\) bands show the same behavior. Using the \(u-r\) color to split the galaxy sample into red and blue galaxies, we show that the changes observed as a function of the system mass are mainly seen in the red, passively evolving, galaxy population, while the luminosities of blue galaxies remain almost unchanged with mass. Finally, we observe that groups having an important luminosity difference between the two brightest galaxies of a system show a steeper faint end slope than the other groups. Our results can be interpreted in terms of galaxy mergers as the main driving force behind galaxy evolution in groups.
Mon.Not.Roy.Astron.Soc.326:147,2001 We compute the redshift space power spectrum of two X-ray cluster samples:
the X-ray Brightest Abell Cluster Sample (XBACS) and the Brightest Cluster
Sample (BCS) ...using the method developed by Feldman, Kaiser & Peacock. The power
spectrums derived for these samples are in agreement with determinations of
other optical and X-ray cluster samples. For XBACS we find the largest power
spectrum amplitude expected given the high richness of this sample ($R \ge 2$).
In the range $0.05 \uk < k < 0.4 \uk$ the power spectrum shows a power law
behavior $P(k)\propto k^{n}$ with an index $n\simeq-1.2$. In a similar range
$0.04 \uk < k < 0.3 \uk $ BCS power spectrum has a smaller amplitude with index
$n\simeq-1.0$. We do not find significant evidence for a peak at $k \simeq 0.05
\uk$ suggesting that claims such of feature detections in some cluster samples
could relay on artificial inhomogeneities of the data. We compare our results
with power spectrum predictions derived by Moscardini et al. within current
cosmological models (LCDM and OCDM). For XBACS we find that both models
underestimate the amplitude of the power spectrum but for BCS there is
reasonably good agreement at $k\gsim 0.03 \uk$ for both models.
We have analysed the distribution of galaxies in groups identified in the largest redshift surveys at the present: the final release of the 2dF Galaxy Redshift Survey and the first release of the ...Sloan Digital Sky Survey. Our work comprises the study of the galaxy density profiles and the fraction of galaxies per spectral type as a function of the group-centric distance. We have calculated the projected galaxy density profiles of galaxy groups using composite samples in order to increase the statistical significance of the results. Special cares have been taken in order to avoid possible biases in the group identification and the construction of the projected galaxy density profile estimator. The results show that the projected galaxy density profiles obtained for both redshift surveys are in agreement with a projected Navarro, Frenk & White predictions in the range \(0.15< r/r_{200} < 1\), whereas a good fit for the measured profiles in the whole range of \(r/r_{200}\) is given by a projected King profile. We have adopted a generalized King profile to fit the measured projected density profiles per spectral type. In order to infer the 3-D galaxy density profiles, we deproject the 2-D density profiles using a deprojection method similar to the developed by Allen & Fabian. From 2-D and 3-D galaxy density profiles we have estimated the corresponding galaxy fractions per spectral type. The 2-D fraction of galaxies computed using the projected profiles show a similar segregation of galaxy spectral types as the obtained by Dom\'ınguez et al. for groups in the early data release of the 2dF Galaxy Redshift Survey. As expected, the trends obtained for the 3-D galaxy fractions show steeper slopes than the observed in the 2-D fractions.
We use the 2dF Galaxy Group Catalogue constructed by Merchán & Zandivarez to study the large scale structure of the Universe traced by galaxy groups. We concentrate on the computation of the power ...spectrum and the two point correlation function. The resulting group power spectrum shows a similar shape to the galaxy power spectrum obtained from the 2dF Galaxy Redshift Survey by Percival et al., but with a higher amplitude quantified by a relative bias in redshift space of \(b_s(k) \sim 1.5\) . The group two point correlation function for the total sample is well described by a power law with correlation length \(s_0=8.9 \pm 0.3 \mpc\) and slope \(\gamma=-1.6 \pm 0.1\) on scales \(s < 20 \mpc\). In order to study the dependence of the clustering properties on group mass we split the catalogue in four subsamples defined by different ranges of group virial masses. These computations allow a fair estimate of the relation described by the correlation length \(s_0\) and the mean intergroup separation \(d_c\) for galaxy systems of low mass. We also extend our study to the redshift space distortions of galaxy groups, where we find that the anisotropies in the clustering pattern of the 2dF group catalogue are consistent with gravitational instability, with a flattening of the redshift-space correlation function contours in the direction of the line of sight.
We compute the redshift space power spectrum of two X-ray cluster samples: the X-ray Brightest Abell Cluster Sample (XBACS) and the Brightest Cluster Sample (BCS) using the method developed by ...Feldman, Kaiser & Peacock. The power spectrums derived for these samples are in agreement with determinations of other optical and X-ray cluster samples. For XBACS we find the largest power spectrum amplitude expected given the high richness of this sample (\(R \ge 2\)). In the range \(0.05 \uk < k < 0.4 \uk\) the power spectrum shows a power law behavior \(P(k)\propto k^{n}\) with an index \(n\simeq-1.2\). In a similar range \(0.04 \uk < k < 0.3 \uk \) BCS power spectrum has a smaller amplitude with index \(n\simeq-1.0\). We do not find significant evidence for a peak at \(k \simeq 0.05 \uk\) suggesting that claims such of feature detections in some cluster samples could relay on artificial inhomogeneities of the data. We compare our results with power spectrum predictions derived by Moscardini et al. within current cosmological models (LCDM and OCDM). For XBACS we find that both models underestimate the amplitude of the power spectrum but for BCS there is reasonably good agreement at \(k\gsim 0.03 \uk\) for both models.
