162 research outputs found
The Hawaii K-Band Galaxy Survey. II. Bright K-band Imaging
We present the results of a wide-field K-selected galaxy survey with
complementary optical I- and B-band imaging in six fields with a total coverage
of 9.8 square degrees. This survey establishes the bright-end K-band galaxy
number counts in the magnitude range 13<K<16 with high precision. We find that
our bright-end counts have a significantly steeper slope than the prediction of
a no-evolution model, which cannot be accounted for by known observational or
theoretical error. We also argue against the likelihood of sufficient evolution
at such low redshifts to account for this effect, we describe an alternative
picture in which there is a local deficiency of galaxies by a factor of 2 on
scale sizes of around 300 Mpc. Taken at face value, this would imply that local
measurements of \Omega_0 underestimate the true value of the cosmological mass
density by this factor and that local measurements of could be high by as
much as 33%.Comment: 24 pages Latex + 8 PostScript figures, to appear in Astrophysical
Journal(02/97
The Aquarius Superclusters - I. Identification of Clusters and Superclusters
We study the distribution of galaxies and galaxy clusters in a 10^deg x 6^deg
field in the Aquarius region. In addition to 63 clusters in the literature, we
have found 39 new candidate clusters using a matched-filter technique and a
counts-in-cells analysis. From redshift measurements of galaxies in the
direction of these cluster candidates, we present new mean redshifts for 31
previously unobserved clusters, while improved mean redshifts are presented for
35 other systems. About 45% of the projected density enhancements are due to
the superposition of clusters and/or groups of galaxies along the line of
sight, but we could confirm for 72% of the cases that the candidates are real
physical associations similar to the ones classified as rich galaxy clusters.
On the other hand, the contamination due to galaxies not belonging to any
concentration or located only in small groups along the line of sight is ~ 10%.
Using a percolation radius of 10 h^{-1} Mpc (spatial density contrast of about
10), we detect two superclusters of galaxies in Aquarius, at z = 0.086 and at z
= 0.112, respectively with 5 and 14 clusters. The latter supercluster may
represent a space overdensity of about 160 times the average cluster density as
measured from the Abell et al. (1989) cluster catalog, and is possibly
connected to a 40 h^{-1} Mpc filament from z ~ 0.11 to 0.14.Comment: LateX text (21 pages) and 12 (ps/eps/gif) figures; figures 5a, 5b and
6 are not included in the main LateX text; to be published in the
Astronomical Journal, March issu
A Quantitative Evaluation of the Galaxy Component of COSMOS and APM Catalogs
We have carried out an independent quantitative evaluation of the galaxy
component of the "COSMOS/UKST Southern Sky Object Catalogue" (SSC) and the
"APM/UKST J Catalogue" (APM). Using CCD observations our results corroborate
the accuracy of the photometry of both catalogs, which have an overall
dispersion of about 0.2 mag in the range 17 <= b_J <= 21.5. The SSC presents
externally calibrated galaxy magnitudes that follow a linear relation, while
the APM instrumental magnitudes of galaxies, only internally calibrated by the
use of stellar profiles, require second-order corrections. The completeness of
both catalogs in a general field falls rapidly fainter than b_J = 20.0, being
slightly better for APM. The 90% completeness level of the SSC is reached
between b_J = 19.5 and 20.0, while for APM this happens between b_J = 20.5 and
21.0. Both SSC and APM are found to be less complete in a galaxy cluster field.
Galaxies misclassified as stars in the SSC receive an incorrect magnitude
because the stellar ones take saturation into account besides using a different
calibration curve. In both cases, the misclassified galaxies show a large
diversity of colors that range from typical colors of early-types to those of
blue star-forming galaxies. A possible explanation for this effect is that it
results from the combination of low sampling resolutions with properties of the
image classifier for objects with characteristic sizes close to the
instrumental resolution. We find that the overall contamination by stars
misclassified as galaxies is < 5% to b_J = 20.5, as originally estimated for
both catalogs. Although our results come from small areas of the sky, they are
extracted from two different plates and are based on the comparison with two
independent datasets.Comment: 14 pages of text and tables, 8 figures; to be published in the
Astronomical Journal; for a single postscript version file see
ftp://danw.on.br/outgoing/caretta/caretta.p
The Northern Sky Optical Cluster Survey II: An Objective Cluster Catalog for 5800 Square Degrees
We present a new, objectively defined catalog of candidate galaxy clusters
based on the galaxy catalogs from the Digitized Second Palomar Observatory Sky
Survey (DPOSS). This cluster catalog, derived from the best calibrated plates
in the high latitude (|b|>30) Northern Galactic Cap region, covers 5,800 square
degrees, and contains 8,155 candidate clusters. A simple adaptive kernel
density mapping technique, combined with the SExtractor object detection
algorithm, is used to detect galaxy overdensities, which we identify as
clusters. Simulations of the background galaxy distribution and clusters of
varying richnesses and redshifts allow us to optimize detection parameters, and
measure the completeness and contamination rates for our catalog. Cluster
richnesses and photometric redshifts are measured, using integrated colors and
magnitudes for each cluster. An extensive spectroscopic survey is used to
confirm the photometric results.
This catalog, with well-characterized sample properties, provides a sound
basis for future studies of cluster physics and large scale structure.Comment: 49 pages, 16 figures. Accepted to AJ; appearing in April. Version
with full resolution figures, and full length tables available at
http://dposs.caltech.edu:8080/NoSOCS.htm
The ROSAT All-Sky Survey: a Catalog of Clusters of Galaxies in a Region of 1 Ster around the South Galactic Pole
A field of 1.013 ster in the ROSAT all-sky survey (RASS), centered on the
south galactic pole (SGP), has been searched in a systematic, objective manner
for clusters of galaxies. The procedure relied on a correlation of the X-ray
positions and properties of ROSAT sources with the distribution of galaxies in
the COSMOS digitised data base, which was obtained by scanning the plates of
the UK Schmidt IIIa-J optical southern sky survey. The study used the second
ROSAT survey data base (RASS-2) and included several optical observing
campaigns to measure redshifts. The search, a precursor to the larger REFLEX
survey of the whole southern sky, reached the detection limits of the RASS and
the COSMOS data, and yielded a catalog of 186 clusters in which the lowest flux
is 1.5e-12 erg/cm2/s in the 0.1-2.4 keV band. Of these 157 have measured
redshifts. Using a limit of 3.0e-12 erg/cm2/s a complete subset of 112 clusters
was obtained, of which 110 have measured redshifts. The spatial distribution of
the X-ray clusters out to z = 0.15 shows an extension of the Local Supercluster
to the Pisces-Cetus supercluster (z<~0.07), and a more distant orthogonal
structure at 0.07<z<0.15.Comment: To be published in ApJ Supplements in February 2002: 53 pages: 18
figure
A Flux-limited Sample of Bright Clusters of Galaxies from the Southern Part of the ROSAT All-Sky Survey: the Catalog and the LogN-LogS
We describe the selection of an X-ray flux-limited sample of bright clusters
of galaxies in the southern hemisphere, based on the first analysis of the
ROSAT All-Sky Survey data (RASS1). The sample is constructed starting from an
identification of candidate clusters in RASS1, and their X-ray fluxes are
remeasured using the Steepness Ratio Technique. This method is better suited
than the RASS1 standard algorithm for measuring flux from extended sources. The
final sample is count-rate-limited in the ROSAT hard band (0.5-2.0 keV), so
that due to the distribution of NH, its effective flux limit varies between
about 3-4 x 10**-12 ergs cm**-2 s**-1 over the selected area. This covers the
Decl<2.5 deg part of the south Galactic cap region (b<-20 deg) - with the
exclusion of patches of low RASS1 exposure time and of the Magellanic Clouds
area - for a total of 8235 deg**2. 130 candidate sources fulfill our selection
criteria for bonafide clusters of galaxies in this area. Of these, 101 are
Abell/ACO clusters, while 29 do not have a counterpart in these catalogs. Of
these clusters, 126 (97%) clusters have a redshift and for these we compute an
X-ray luminosity. 20% of the cluster redshifts come from new observations, as
part of the ESO Key Program REFLEX Cluster Survey that is under completion.
Considering the intrinsic biases and incompletenesses introduced by the flux
selection and source identification processes, we estimate the overall
completeness to be better than 90%. The observed number count distribution,
LogN-LogS, is well fitted by a power law with slope alpha = 1.34 +/- 0.15 and
normalization A = 11.87 +/- 1.04 sr**-1 (10**-11 ergs cm**-2 s**-1)**alpha, in
good agreement with other measurements.Comment: 27 pages, 8 figures and 3 tables included, LaTex, emulateapj.sty and
epsf.sty, accepted for publication in ApJ: scheduled for the March 20, 1999,
Vol.514. The cluster catalog is available at
http://www.merate.mi.astro.it/~degrand
The Nearby Optical Galaxy Sample: The Local Galaxy Luminosity Function
In this paper we derive the galaxy luminosity function from the Nearby
Optical Galaxy (NOG) sample, which is a nearly complete, magnitude-limited
(B<14 mag), all-sky sample of nearby optical galaxies (~6400 galaxies with
cz<5500 km/s). For this local sample, we use galaxy distance estimates based on
different peculiar velocity models. Therefore, the derivation of the luminosity
function is carried out using the locations of field and grouped galaxies in
real distance space.
The local field galaxy luminosity function in the B system is well described
by a Schechter function. The exact values of the Schechter parameters slightly
depend on the adopted peculiar velocity field models.
The shape of the luminosity function of spiral galaxies does not differ
significantly from that of E-S0 galaxies. On the other hand, the late-type
spirals and irregulars have a very steeply rising luminosity function towards
the faint end, whereas the ellipticals appreciably decrease in number towards
low luminosities.
The presence of galaxy systems in the NOG sample does not affect
significantly the field galaxy luminosity function, since environmental effects
on the total luminosity function appear to be marginal.Comment: 35 pages including 7 figures and 4 tables. Accepted for publication
in Ap
Comparative Clinical Performance Of Two Silicone Hydrogel Contact Lenses For Continuous Wear
BACKGROUND: Silicone hydrogel soft contact lenses are now available for use on a 30-day continuous wear basis. The aim of this study was to compare the clinical performance of two such lenses. METHODS: In a single-centre, randomised, subject-masked, two-period crossover study, 30 subjects wore a pair of PureVision lenses (Bausch & Lomb) and a pair of Focus Night & Day lenses (CIBA Vision), alternately, for successive eight-week periods. Assessment was made of lens fit and surface characteristics, logMAR visual acuity, ocular response and subjective reaction. RESULTS: Lens fit, deposition and post-lens debris were similar for the two lens types. High contrast visual acuity was statistically significantly better for the PureVision lens, as was the subject-reported quality of vision, although these differences were not considered clinically significant. For both lenses, limbal and conjunctival redness reduced throughout the duration of the study, whereas there was a slight increase in the overall amount of corneal staining. The incidence of mucin balls peaked four weeks after commencing lens wear and began to decline thereafter; more mucin balls were noticed in subjects wearing Focus Night & Day lenses. No differences between the lenses were observed for any other biomicroscopic signs. CONCLUSIONS: This study demonstrates similar clinical performance with the two silicone hydrogel lenses evaluated. We believe that, with careful monitoring, both of these new-generation lenses can be prescribed for continuous wear
Faint galaxy population in clusters: X-ray emission, cD halos and projection effects
We analyze samples of nearby clusters taken from the Abell catalog and the
X-ray Sample of Bright Clusters(De Grandi et al 1999) including a wide range of
X-ray luminosities.Using the usually adopted background subtraction procedures,
we find that galaxies in clusters selected by means of their X-ray emission
show a flat luminosity function (faint end slope )
consistent with that derived for galaxies in the field and groups. By contrast,
the sample of Abell clusters that do not have an X-ray counterpart shows a
galaxy luminosity function with a steep faint end (). We
investigate the possibility that cD halos could be formed by the disruption of
galaxies in rich relaxed clusters that show an apparently flat faint end galaxy
luminosity function (Lopez-Cruz et al 1997).
We find that clusters dominated by a central cD galaxy (Bautz-Morgan classes
I and II) show the same systematic trend: X-ray selected clusters have flatter
faint end slopes than those clusters with no detected X-ray emission. Thus, it
is likely the X-ray selection and not the cluster domination by central
galaxies what correlates with background decontamination estimates of the
galaxy luminosity function. Moreover, no significant correlation between X-ray
luminosity and the galaxy LF faint end slope is found. These results do not
support a scenario where flat faint end slopes are a consequence of cD
formation via the disruption of faint galaxies. We argue that the clusters
without X-ray emission are strongly affected by projection effects which give
rise to spurious faint end slopes estimated using background subtraction
procedures (Valotto et al 2001).Comment: Accepted for publication in ApJ (vol. 601
Do clusters contain a large population of dwarf galaxies?
We analyze systematic effects in the determination of the galaxy luminosity
function in clusters using a deep mock catalogue constructed from a numerical
simulation of a hierarchical universe. The results indicate a strong tendency
to derive a rising faint end (\alpha \lsim -1.5) in clusters selected in two
dimensions, using a galaxy catalogue constructed with a universal flat
luminosity function with . This is due to the projection
effects inherent in catalogues of clusters constructed using 2 dimensional
data. Many of the clusters found in 2d have no significant 3d counterparts, and
most suffer from massive background contamination that cannot be corrected for
by subtracting random offset fields. The luminosity function of high surface
brightness galaxies in the field and within small groups follows a Schechter
function with a fairly flat faint end slope, with
to -1.2. On the contrary, observational studies of clusters
constructed using Abell, EDCC and APM catalogues are systematically found to
have steeper luminosity functions with to -2.0. This may be
attributed to projection effects rather than a dominant population of high
surface brightness dwarf galaxies (M\gsim M^*+2) in clusters. It should be
straighforward to confirm our results by measuring redshifts of these faint
cluster galaxies.Comment: 23 pages, 7 Postscript figures TeX, accepted for publication in the
Astrophysical Journal, e-mail:[email protected]
http://iate.oac.uncor.edu/cv.htm
- …