105 research outputs found
Large-Scale Structure in the NIR-Selected MUNICS Survey
The Munich Near-IR Cluster Survey (MUNICS) is a wide-area, medium-deep,
photometric survey selected in the K' band. The project's main scientific aims
are the identification of galaxy clusters up to redshifts of unity and the
selection of a large sample of field early-type galaxies up to z < 1.5 for
evolutionary studies. We created a Large Scale Structure catalog, using a new
structure finding technique specialized for photometric datasets, that we
developed on the basis of a friends-of-friends algorithm. We tested the
plausibility of the resulting galaxy group and cluster catalog with the help of
Color-Magnitude Diagrams (CMD), as well as a likelihood- and Voronoi-approach.Comment: 4 pages, to appear in "The Evolution of Galaxies III. From Simple
Approaches to Self-Consistent Models", proceedings of the 3rd EuroConference
on the evolution of galaxies, held in Kiel, Germany, July 16-20, 200
The Munich Near-Infrared Cluster Survey - I. Field selection, object extraction, and photometry
The Munich Near-IR Cluster Survey (MUNICS) is a wide-area, medium-deep,
photometric survey selected in the K' band. It covers an area of roughly one
square degree in the K' and J near-IR pass-bands. The survey area consists of
16 6' x 6' fields targeted at QSOs with redshifts 0.5 < z < 2 and 7 28' x 13'
stripes targeted at `random' high Galactic latitude fields. Ten of the QSO
fields were additionally imaged in R and I, and 0.6 square degrees of the
randomly selected fields were also imaged in the V, R, and I bands. The
resulting object catalogues were strictly selected in K', having a limiting
magnitude (50 per cent completeness) of K' ~ 19.5 mag and J ~ 21 mag,
sufficiently deep to detect passively evolving systems up to a redshift of z ~
1.5 and luminosity of 0.5 L*. The optical data reach a depth of roughly R ~
23.5 mag. The project's main scientific aims are the identification of galaxy
clusters at redshifts around unity and the selection of a large sample of field
early-type galaxies at 0 < z < 1.5 for evolutionary studies. In this paper -
the first in a series - we describe the survey's concept, the selection of the
survey fields, the near-IR and optical imaging and data reduction, object
extraction, and the construction of photometric catalogues. Finally, we show
the J-K' vs. K' colour-magnitude diagramme and the R-J vs. J-K', V-I vs. J-K',
and V-I vs. V-R colour-colour diagrammes for MUNICS objects, together with
stellar population-synthesis models for different star-formation histories, and
conclude that the data set presented is suitable for extracting a catalogue of
massive field galaxies in the redshift range 0.5 < z < 1.5 for evolutionary
studies and follow-up observations.Comment: Accepted for publication in MNRA
Microlens OGLE-2005-BLG-169 Implies Cool Neptune-Like Planets are Common
We detect a Neptune mass-ratio (q~8e-5) planetary companion to the lens star
in the extremely high-magnification (A~800) microlensing event
OGLE-2005-BLG-169. If the parent is a main-sequence star, it has mass M~0.5
M_sun implying a planet mass of ~13 M_earth and projected separation of ~2.7
AU. When intensely monitored over their peak, high-magnification events similar
to OGLE-2005-BLG-169 have nearly complete sensitivity to Neptune mass-ratio
planets with projected separations of 0.6 to 1.6 Einstein radii, corresponding
to 1.6--4.3 AU in the present case. Only two other such events were monitored
well enough to detect Neptunes, and so this detection by itself suggests that
Neptune mass-ratio planets are common. Moreover, another Neptune was recently
discovered at a similar distance from its parent star in a low-magnification
event, which are more common but are individually much less sensitive to
planets. Combining the two detections yields 90% upper and lower frequency
limits f=0.37^{+0.30}_{-0.21} over just 0.4 decades of planet-star separation.
In particular, f>16% at 90% confidence. The parent star hosts no Jupiter-mass
companions with projected separations within a factor 5 of that of the detected
planet. The lens-source relative proper motion is \mu~7--10 mas/yr, implying
that if the lens is sufficiently bright, I<23.8, it will be detectable by HST
by 3 years after peak. This would permit a more precise estimate of the lens
mass and distance, and so the mass and projected separation of the planet.
Analogs of OGLE-2005-BLG-169Lb orbiting nearby stars would be difficult to
detect by other methods of planet detection, including radial velocities,
transits, or astrometry.Comment: Submitted to ApJ Letters, 9 text pages + 4 figures + 1 tabl
A wide angle tail radio galaxy in the COSMOS field: evidence for cluster formation
We have identified a complex galaxy cluster system in the COSMOS field via a
wide angle tail (WAT) radio galaxy consistent with the idea that WAT galaxies
can be used as tracers of clusters. The WAT galaxy, CWAT-01, is coincident with
an elliptical galaxy resolved in the HST-ACS image. Using the COSMOS
multiwavelength data set, we derive the radio properties of CWAT-01 and use the
optical and X-ray data to investigate its host environment. The cluster hosting
CWAT-01 is part of a larger assembly consisting of a minimum of four X-ray
luminous clusters within ~2 Mpc distance. We apply hydrodynamical models that
combine ram pressure and buoyancy forces on CWAT-01. These models explain the
shape of the radio jets only if the galaxy's velocity relative to the
intra-cluster medium (ICM) is in the range of about 300-550 km/s which is
higher than expected for brightest cluster galaxies (BCGs) in relaxed systems.
This indicates that the CWAT-01 host cluster is not relaxed, but is possibly
dynamically young. We argue that such a velocity could have been induced
through subcluster merger within the CWAT-01 parent cluster and/or
cluster-cluster interactions. Our results strongly indicate that we are
witnessing the formation of a large cluster from an assembly of multiple
clusters, consistent with the hierarchical scenario of structure formation. We
estimate the total mass of the final cluster to be approximately 20% of the
mass of the Coma cluster.Comment: 18 pages, 13 figures; accepted for publication in ApJS, COSMOS
special issue; added color figure (Fig. 13) which was previously unavailabl
Integrated specific star formation rates of galaxies, groups, and clusters: A continuous upper limit with stellar mass?
Aims: We investigate the build-up of stellar mass through star formation in
field galaxies, galaxy groups, and clusters in order to better understand the
physical processes regulating star formation in different haloes.
Methods: In order to do so we relate ongoing star formation activity to the
stellar mass by studying the integrated specific star formation rate (SSFR),
defined as the star-formation rate per unit stellar mass, as a function of
integrated stellar mass for samples of field galaxies, groups of galaxies, and
galaxy clusters at 0.18 < z < 0.85. The star formation rate (SFR) is derived
from the ultraviolet continuum for the galaxies and group members, and from
emission line fluxes for the cluster galaxies. The stellar masses are computed
from multi-band photometry including the near-infrared bands for the galaxies
and groups, and from the dynamical mass for the cluster sample.
Results: For the first time, integrated SSFRs for clusters and groups are
presented and related to the SSFRs of field galaxies. Tentatively, we find a
continuous upper limit for galaxies, groups, and clusters in the SSFR-stellar
mass plane over seven orders of magnitude in stellar mass. This might indicate
that the physical processes which control star formation in dark matter haloes
of different mass have the same scaling with mass over a wide range of masses
from dwarf galaxies to massive clusters of galaxies.Comment: Accepted for publication in A&A Letters; 4 pages, 1 figur
Determining the Physical Lens Parameters of the Binary Gravitational Microlensing Event MOA-2009-BLG-016
We report the result of the analysis of the light curve of the microlensing
event MOA-2009-BLG-016. The light curve is characterized by a short-duration
anomaly near the peak and an overall asymmetry. We find that the peak anomaly
is due to a binary companion to the primary lens and the asymmetry of the light
curve is explained by the parallax effect caused by the acceleration of the
observer over the course of the event due to the orbital motion of the Earth
around the Sun. In addition, we detect evidence for the effect of the finite
size of the source near the peak of the event, which allows us to measure the
angular Einstein radius of the lens system. The Einstein radius combined with
the microlens parallax allows us to determine the total mass of the lens and
the distance to the lens. We identify three distinct classes of degenerate
solutions for the binary lens parameters, where two are manifestations of the
previously identified degeneracies of close/wide binaries and positive/negative
impact parameters, while the third class is caused by the symmetric cycloid
shape of the caustic. We find that, for the best-fit solution, the estimated
mass of the lower-mass component of the binary is (0.04 +- 0.01) M_sun,
implying a brown-dwarf companion. However, there exists a solution that is
worse only by \Delta\chi^2 ~ 3 for which the mass of the secondary is above the
hydrogen-burning limit. Unfortunately, resolving these two degenerate solutions
will be difficult as the relative lens-source proper motions for both are
similar and small (~ 1 mas/yr) and thus the lens will remain blended with the
source for the next several decades.Comment: 7 pages, 2 tables, and 5 figure
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