scholarly journals Effects of Sampling on Measuring Galaxy Count Probabilities

1996 ◽  
Vol 459 ◽  
pp. 504 ◽  
Author(s):  
Istvan Szapudi ◽  
Alexander S. Szalay
Keyword(s):  
Galaxy Count

scholarly journals Searching for cross-correlation between stochastic gravitational-wave background and galaxy number counts

2020 ◽  
Vol 500 (2) ◽  
pp. 1666-1672
Author(s):  
Kate Z Yang ◽  
Vuk Mandic ◽  
Claudia Scarlata ◽  
Sharan Banagiri
Keyword(s):  
Gravitational Wave ◽  
Cross Correlation ◽  
Sloan Digital Sky Survey ◽  
Number Count ◽  
Frequency Bands ◽  
Galaxy Count ◽  
Harmonic Decomposition ◽  
Number Counts ◽  
Gravitational Wave Background ◽  
The Universe

ABSTRACT Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO) and Advanced Virgo have recently published the upper limit measurement of persistent directional stochastic gravitational-wave background (SGWB) based on data from their first and second observing runs. In this paper, we investigate whether a correlation exists between this maximal likelihood SGWB map and the electromagnetic (EM) tracers of matter structure in the Universe, such as galaxy number counts. The method we develop will improve the sensitivity of future searches for anisotropy in the SGWB and expand the use of SGWB anisotropy to probe the formation of structure in the Universe. In order to compute the cross-correlation, we used the spherical harmonic decomposition of SGWB in multiple frequency bands and converted them into pixel-based sky maps in healpix basis. For the EM part, we use the Sloan Digital Sky Survey alaxy catalogue and form healpix sky maps of galaxy number counts at the same angular resolution as the SGWB maps. We compute the pixel-based coherence between these SGWB and galaxy count maps. After evaluating our results in different SGWB frequency bands and in different galaxy redshift bins, we conclude that the coherence between the SGWB and galaxy number count maps is dominated by the null measurement noise in the SGWB maps, and therefore not statistically significant. We expect the results of this analysis to be significantly improved by using the more sensitive upcoming SGWB measurements based on the third observing run of Advanced LIGO and Advanced Virgo.

The Application of the Study of Galaxies Associated With Quasars to Observational Cosmology

1987 ◽  
Vol 124 ◽  
pp. 685-689
Author(s):  
H.K.C. Yee
Keyword(s):  
Galaxy Clusters ◽  
Count Data ◽  
Luminosity Function ◽  
Current Data ◽  
Observational Cosmology ◽  
Direct Imaging ◽  
Large Uncertainty ◽  
Self Consistent ◽  
Galaxy Count

CCD direct imaging of fields around quasars is used as a method for locating galaxy clusters and groups associated with quasars. Average galaxy counts in the sky obtained from control fields are used to correct for background galaxies in the quasar fields. This correction allows one to derive the luminosity function (LF) of the associated galaxies at the redshifts of the quasars. It is demonstrated that using the derived LF and average galaxy count data, self-consistent models of the evolution of the LF and galaxy counts can be obtained. Current data are best fitted, with a large uncertainty, by a qo between 0.0 and 0.5 and an evolution in M* of −0.9±0.5 mag. It is found that the average environment of radio-loud quasars at z∼0.6 is about three times richer in galaxies than that of quasars at z∼0.4.

Deep galaxy count predictions in the radio, infrared, and X-ray spectral bands

1993 ◽  
Vol 408 ◽  
pp. L1 ◽  
Author(s):  
Marie-Agnes Treyer ◽  
Joseph Silk
Keyword(s):  
X Ray ◽  
Spectral Bands ◽  
Galaxy Count

scholarly journals Constraints on Far-Infrared Source Counts in the Lockman Hole using a Power Spectrum Analysis

2001 ◽  
Vol 204 ◽  
pp. 301-301
Author(s):  
H. Matsuhara ◽  
K. Kawara ◽  
Y. Sofue ◽  
Y. Taniguchi ◽  
Y. Sato ◽  
...  
Keyword(s):  
Background Radiation ◽  
Power Spectra ◽  
Far Infrared ◽  
Infrared Space Observatory ◽  
Infrared Source ◽  
Star Forming ◽  
The Galaxy ◽  
Galaxy Count ◽  
Infrared Background ◽  
Lockman Hole

We present the characteristics of far-infrared (FIR) brightness fluctuations at 90 μm and 170 μm in the Lockman Hole, which were surveyed with the ISOPHOT instrument aboard the Infrared Space Observatory (ISO), and give constraints on the galaxy number counts down to 30 mJy at 90 μm and 50 mJy at 170 μm. The fluctuation power spectra of the FIR images are not dominated by IR cirrus, and are instead most likely due to star-forming galaxies. This analysis indicates the existence of strong evolution in the counts. Especially at 90 μm, the source density is much larger than that expected from the currently available galaxy count models. The galaxies responsible for the fluctuations also significantly contribute to the cosmic infrared background radiation recently derived from an analysis of the COBE data.

scholarly journals The Galaxy Count Correlation Function in Redshift Space Revisited

2017 ◽  
Vol 845 (1) ◽  
pp. 28 ◽  
Author(s):  
J.-E. Campagne ◽  
S. Plaszczynski ◽  
J. Neveu
Keyword(s):  
Correlation Function ◽  
The Galaxy ◽  
Galaxy Count

Faint blue galaxy count and the dwarf population of starburst galaxies

1995 ◽  
Vol 19 (4) ◽  
pp. 405-413
Author(s):  
Shi Chen ◽  
Er Ma ◽  
Yun-qiang Yu
Keyword(s):  
Starburst Galaxies ◽  
Galaxy Count ◽  
Blue Galaxy

scholarly journals Simulating galaxy formation in f(R) modified gravity: matter, halo, and galaxy statistics

2019 ◽  
Vol 490 (2) ◽  
pp. 2507-2520 ◽  
Author(s):  
Christian Arnold ◽  
Baojiu Li
Keyword(s):  
Correlation Function ◽  
Power Spectrum ◽  
Galaxy Formation ◽  
Mass Function ◽  
Back Reaction ◽  
Satellite Galaxy ◽  
Matter Power Spectrum ◽  
Hydrodynamical Simulation ◽  
The Galaxy ◽  
Galaxy Count

ABSTRACT We present an analysis of the matter, halo, and galaxy clustering in f(R)-gravity employing the SHYBONE full-physics hydrodynamical simulation suite. Our analysis focuses on the interplay between baryonic feedback and f(R)-gravity in the matter power spectrum, the matter and halo correlation functions, the halo and galaxy–host–halo mass function, the subhalo and satellite–galaxy count, and the correlation function of the stars in our simulations. Our studies of the matter power spectrum in full-physics simulations in f(R)-gravity show that it will be very difficult to derive accurate fitting formulae for the power spectrum enhancement in f(R)-gravity which include baryonic effects. We find that the enhancement of the halo mass function due to f(R)-gravity and its suppression due to feedback effects do not show significant back-reaction effects and can thus be estimated from independent general relativity-hydro and f(R) dark matter only simulations. Our simulations furthermore show that the number of subhaloes and satellite-galaxies per halo is not significantly affected by f(R)-gravity. Low-mass haloes are nevertheless more likely to be populated by galaxies in f(R)-gravity. This suppresses the clustering of stars and the galaxy correlation function in the theory compared to standard cosmology.

scholarly journals The very bright SCUBA galaxy count: looking for SCUBA galaxies with the Mexican hat wavelet

2004 ◽  
Vol 352 (3) ◽  
pp. 961-974 ◽  
Author(s):  
V. E. Barnard ◽  
P. Vielva ◽  
D. P. I. Pierce-Price ◽  
A. W. Blain ◽  
R. B. Barreiro ◽  
...  
Keyword(s):  
Mexican Hat Wavelet ◽  
Mexican Hat ◽  
Galaxy Count

scholarly journals K-band Extragalactic Background Light from Deep Galaxy Counts in the Subaru Deep Field

2001 ◽  
Vol 204 ◽  
pp. 119-119
Author(s):  
T. Totani ◽  
Y. Yoshii ◽  
F. Iwamuro ◽  
T. Maihara ◽  
K. Motohara ◽  
...  
Keyword(s):  
Count Data ◽  
Integration Time ◽  
Selection Effects ◽  
Significant Discrepancy ◽  
Extragalactic Background Light ◽  
Background Light ◽  
Systematic Uncertainties ◽  
Galaxy Count ◽  
Total Integration ◽  
K Band

We report estimates for the extragalactic background light (EBL) in the K band (2.2 μm), obtained by the integration of galaxy counts down to K=25 mag in the Subaru Deep Field (SDF, 2′ x 2′). We have obtained deep galaxy count data by using the 8.2m Subaru telescope, with a total integration time of 10 hours and an average seeing of about 0.4 arcsec. The 5-sigma limiting magnitude is K=23.5, and 350 objects are detected brighter than this magnitude. There has been a significant discrepancy between previous K-count observations, probably because of the systematic uncertainties in the completeness correction. To overcome this problem, we have paid special attention to selection effects and completeness corrections, with realistic theoretical galaxy models taken into account consistently. The faint-end slope is significantly flatter than some earlier observations of K counts, and our results suggest that the bulk of the extragalactic light in this band has been resolved as discrete sources. We estimate the value of the EBL flux obtained from the integration of our counts as 9.8 ± 1.0 nWm−2 sr−1.

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