102 research outputs found
The Munich Near-Infrared Cluster Survey -- IV. Biases in the Completeness of Near-Infrared Imaging Data
We present the results of completeness simulations for the detection of point
sources as well as redshifted elliptical and spiral galaxies in the K'-band
images of the Munich Near-Infrared Cluster Survey (MUNICS). The main focus of
this work is to quantify the selection effects introduced by threshold-based
object detection algorithms used in deep imaging surveys. Therefore, we
simulate objects obeying the well-known scaling relations between effective
radius and central surface brightness, both for de Vaucouleurs and exponential
profiles. The results of these simulations, while presented for the MUNICS
project, are applicable in a much wider context to deep optical and
near-infrared selected samples. We investigate the detection probability as
well as the reliability for recovering the true total magnitude with Kron-like
(adaptive) aperture photometry. The results are compared to the predictions of
the visibility theory of Disney and Phillipps in terms of the detection rate
and the lost-light fraction. Additionally, the effects attributable to seeing
are explored. The results show a bias against detecting high-redshifted massive
elliptical galaxies in comparison to disk galaxies with exponential profiles,
and that the measurements of the total magnitudes for intrinsically bright
elliptical galaxies are systematically too faint. Disk galaxies, in contrast,
show no significant offset in the magnitude measurement of luminous objects.
Finally we present an analytic formula to predict the completeness of
point-sources using only basic image parameters.Comment: 13 pages, 11 figures, accepted for publication in MNRA
The Mass Function of Field Galaxies at 0.4 < z < 1.2 Derived From the MUNICS K-Selected Sample
We derive the number density evolution of massive field galaxies in the
redshift range 0.4 < z < 1.2 using the K-band selected field galaxy sample from
the Munich Near-IR Cluster Survey (MUNICS). We rely on spectroscopically
calibrated photometric redshifts to determine distances and absolute magnitudes
in the rest-frame K-band. To assign mass-to-light ratios, we use two different
approaches. First, we use an approach which maximizes the stellar mass for any
K-band luminosity at any redshift. We take the mass-to-light ratio of a Simple
Stellar Population (SSP) which is as old as the universe at the galaxy's
redshift as a likely upper limit. Second, we assign each galaxy a mass-to-light
ratio by fitting the galaxy's colours against a grid of composite stellar
population models and taking their M/L. We compute the number density of
galaxies more massive than 2 x 10^10 h^-2 Msun, 5 x 10^10 h^-2 Msun, and 1 x
10^11 h^-2 Msun, finding that the integrated stellar mass function is roughly
constant for the lowest mass limit and that it decreases with redshift by a
factor of ~ 3 and by a factor of ~ 6 for the two higher mass limits,
respectively. This finding is in qualitative agreement with models of
hierarchical galaxy formation, which predict that the number density of ~ M*
objects is fairly constant while it decreases faster for more massive systems
over the redshift range our data probe.Comment: 6 pages, 2 figures, to appear in the proceedings of the ESO/USM
Workshop "The Mass of Galaxies at Low and High Redshift", Venice (Italy),
October 24-26, 200
The Munich Near-Infrared Cluster Survey (MUNICS) - Number density evolution of massive field galaxies to z ~ 1.2 as derived from the K-band selected survey
We derive the number density evolution of massive field galaxies in the
redshift range 0.4 < z < 1.2 using the K-band selected field galaxy sample from
the Munich Near-IR Cluster Survey (MUNICS). We rely on spectroscopically
calibrated photometric redshifts to determine distances and absolute magnitudes
in the rest-frame K-band. To assign mass-to-light ratios, we use an approach
which maximizes the stellar mass for any K-band luminosity at any redshift. We
take the mass-to-light ratio, M/L_K, of a Simple Stellar Population (SSP) which
is as old as the universe at the galaxy's redshift as a likely upper limit.
This is the most extreme case of pure luminosity evolution and in a more
realistic model M/L_K will probably decrease faster with redshift due to
increased star formation. We compute the number density of galaxies more
massive than 2 10^10 h^-2 solar masses, 5 10^10 h^-2 solar masses, and 1 10^11
h^-2 solar masses, finding that the integrated stellar mass function is roughly
constant for the lowest mass limit and that it decreases with redshift by a
factor of roughly 3 and by a factor of roughly 6 for the two higher mass
limits, respectively. This finding is in qualitative agreement with models of
hierarchical galaxy formation, which predict that the number density of ~ M*
objects is fairly constant while it decreases faster for more massive systems
over the redshift range our data probe.Comment: 4 pages, 5 figures, accepted for publication in ApJ Letter
The Munich Near-Infrared Cluster Survey (MUNICS) -- II. The K-Band Luminosity Function of Field Galaxies to z ~ 1.2
(Abriged) We present a measurement of the evolution of the rest-frame K-band
luminosity function to z ~ 1.2 using a sample of more than 5000 K-selected
galaxies drawn from the MUNICS dataset. Distances and absolute K-band
magnitudes are derived using photometric redshifts from spectral energy
distribution fits to BVRIJK photometry. These are calibrated using >500
spectroscopic redshifts. We obtain redshift estimates having a rms scatter of
0.055 and no mean bias. We use Monte-Carlo simulations to investigate the
influence of the errors in distance associated with photometric redshifts on
our ability to reconstruct the shape of the luminosity function. Finally, we
construct the rest-frame K-band LF in four redshift bins spanning 0.4<z<1.2 and
compare our results to the local luminosity function. We discuss and apply two
different estimators to derive likely values for the evolution of the number
density, Phi*, and characteristic luminosity, M*, with redshift. While the
first estimator relies on the value of the luminosity function binned in
magnitude and redshift, the second estimator uses the individually measured
{M,z} pairs alone. In both cases we obtain a mild decrease in number density by
\~ 25% to z=1 accompanied by brightening of the galaxy population by 0.5 to 0.7
mag. These results are fully consistent with an analogous analysis using only
the spectroscopic MUNICS sample. The total K-band luminosity density is found
to scale as dlog(rho_L)/dz = 0.24. We discuss possible sources of systematic
errors and their influence on our parameter estimates.Comment: Accepted for publication in Ap
Dark matter halo properties from galaxy-galaxy lensing
We present results for a galaxy-galaxy lensing study based on imaging data
from the Canada-France-Hawaii Telescope Legacy Survey Wide. From a 12 million
object multi-colour catalogue for 124 deg^2 of photometric data in the
u*g'r'i'z' filters we compute photometric redshifts (with a scatter of
\sigma_{\Delta z/(1+z)} = 0.033 and an outlier rate of \eta=2.0 per cent for
i'<=22.5) and extract galaxy shapes down to i'=24.0. We select a sample of
lenses and sources with 0.05 < z_d <= 1 and 0.05 < z_s <= 2. We fit three
different galaxy halo profiles to the lensing signal, a singular isothermal
sphere (SIS), a truncated isothermal sphere (BBS) and a universal density
profile (NFW). We derive velocity dispersions by fitting an SIS out to 100
h^{-1} kpc to the excess surface mass density \Delta\Sigma and perform maximum
likelihood analyses out to a maximum scale of 2 h^{-1} Mpc to obtain halo
parameters and scaling relations. We find luminosity scaling relations of
\sigma_{red} ~ L^{0.24+-0.03} for the red lens sample, \sigma_{blue} ~
L^{0.23+-0.03} for blue lenses and \sigma ~ L^{0.29+-0.02} for the combined
lens sample with zeropoints of \sigma*_{red}=162+-2 km/s, \sigma*_{blue}=115+-3
km/s and \sigma*=135+-2 km/s at a chosen reference luminosity L*_{r'} = 1.6
\times 10^10 h^{-2} L_{r',sun}. The steeper slope for the combined sample is
due to the different zeropoints of the blue and red lenses and the fact that
blue lenses dominate at low luminosities and red lenses at high luminosities.
The mean effective redshifts for the lens samples are =0.28 for red
lenses, =0.35 for blue lenses and =0.34 for the combined lens
sample.Comment: 62 pages, 55 figures, accepted for publication in MNRAS, abridged
abstract, includes corrections from final proof. Our created catalogues
(photometry, photometric redshifts and shears) are publicly available at
http://www.usm.uni-muenchen.de/people/stella/GGL
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 (MUNICS) - V. The evolution of the rest-frame K-band and J-band galaxy luminosity functions to z ~ 0.7
We present spectroscopic follow-up observations of galaxies from the Munich
Near-Infrared Cluster Survey (MUNICS). MUNICS is a wide-field medium-deep
K'-band selected survey covering 1 square degree in the near-infrared K' and J
pass-bands, and 0.35 square degrees in I, R, V, and - recently completed - B.
The spectroscopic sample comprises observations of objects down to a limit of
K' < 17.5 in five survey fields (0.17 square degrees in total), and a sparsely
selected deeper sample (K' < 19.0) constructed in one of the survey patches
(0.03 square degrees). Here we describe the selection procedure of objects for
spectroscopic observations, the observations themselves, the data reduction,
and the construction of the spectroscopic catalogue containing roughly 500
galaxies with secure redshifts. Furthermore we discuss global properties of the
sample like its distribution in colour-redshift space, the accuracy of redshift
determination, and the completeness function of the data. We derive the
rest-frame K'-band luminosity function of galaxies at median redshifts of z =
0.2, z = 0.4, and z = 0.7. We find evidence for mild evolution of magnitudes
(-0.70 mag) and number densities (35 per cent) to redshift one. Furthermore, we
present the rest-frame J-band luminosity function of galaxies at these
redshifts, the first determination of this quantity at higher redshifts, with a
behaviour similar to the K-band luminosity function.Comment: 18 pages, 15 figures, accepted for publication in MNRAS;
high-resolution versions of Figures 5c-d and 8a-d available on
http://www.usm.uni-muenchen.de/people/feulner/munics5/munics5.htm
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