scholarly journals Global analysis of luminosity- and colour-dependent galaxy clustering in the Sloan Digital Sky Survey

2019 ◽  
Vol 488 (1) ◽  
pp. 1220-1234
Author(s):  
Niladri Paul ◽  
Isha Pahwa ◽  
Aseem Paranjape
Keyword(s):  
Dynamic Range ◽  
Global Analysis ◽  
Spatial Separation ◽  
Sloan Digital Sky Survey ◽  
Independent Manner ◽  
Galaxy Clustering ◽  
Satellite Galaxy ◽  
Sky Survey ◽  
Best Fitting ◽  
Sphere Approximation

ABSTRACT We present a halo occupation distribution (HOD) analysis of the luminosity- and colour-dependent galaxy clustering in the Sloan Digital Sky Survey. A novelty of our technique is that it uses a combination of clustering measurements in luminosity bins to perform a global likelihood analysis, simultaneously constraining the HOD parameters for a range of luminosity thresholds. We present simple, smooth fitting functions which accurately describe the resulting luminosity dependence of the best-fitting HOD parameters. To minimize systematic halo modelling effects, we use theoretical halo 2-point correlation functions directly measured and tabulated from a suite of N-body simulations spanning a large enough dynamic range in halo mass and spatial separation. Thus, our modelling correctly accounts for non-linear and scale-dependent halo bias as well as any departure of halo profiles from universality, and we additionally account for halo exclusion using the hard sphere approximation. Using colour-dependent clustering information, we constrain the satellite galaxy red fraction in a model-independent manner which does not rely on any group-finding algorithm. We find that the resulting luminosity dependence of the satellite red fraction is significantly shallower than corresponding measurements from galaxy group catalogues, and we provide a simple fitting function to describe this dependence. Our fitting functions are readily usable in generating low-redshift mock galaxy catalogues, and we discuss some potentially interesting applications as well as possible extensions of our technique.

scholarly journals Clustering and Halo Occupation Distribution of Active Galactic Nuclei

2013 ◽  
Vol 9 (S304) ◽  
pp. 243-243
Author(s):  
Takamitsu Miyaji ◽  
M. Krumpe ◽  
A. Coil ◽  
H. Aceves ◽  
B. Husemann
Keyword(s):  
Cross Correlation ◽  
Dynamic Range ◽  
Signal To Noise Ratio ◽  
Sloan Digital Sky Survey ◽  
Dark Matter Halo ◽  
Bias Parameter ◽  
X Ray ◽  
Sky Survey ◽  
Galaxy Population ◽  
Halo Occupation Distribution

AbstractWe present the results of our series of studies on correlation function and halo occupation distribution of AGNs utilizing data the ROSAT All-Sky Survey (RASS) and the Sloan Digital Sky Survey (SDSS) in the redshift range of 0.07<z<0.36. In order to improve the signal-to-noise ratio, we take cross-correlation approach, where cross-correlation functions (CCF) between AGNs and much more numerous AGNs are analyzed. The calculated CCFs are analyzed using the Halo Occupation Distribution (HOD) model, where the CCFs are divided into the term contributed by the AGN-galaxy pairs that reside in one dark matter halo (DMH), (the 1-halo term) and those from two different DMHs (the 2-halo term). The 2-halo term is the indicator of the bias parameter, which is a function of the typical mass of the DMHs in which AGNs reside. The combination of the 1-halo and 2-halo terms gives, not only the typical DMH mass, but also how the AGNs are distributed among the DMHs as a function of mass separately for those at the center of the DMHs and satellites. The main results are as follows: (1) the range of typical mass of the DMHs in various sub-samples of AGNs log (MDMH/h−1MΘ) ~ 12.4–13.4, (2) we found a dependence of the AGN bias parameter on the X-ray luminosity of AGNs, while the optical luminosity dependence is not significant probably due to smaller dynamic range in luminosity for the optically-selected sample, and (3) the growth of the number of AGNs per DMH (N (MDMH)) with MDMH is shallow, or even may be flat, contrary to that of the galaxy population in general, which grows with MDMH proportionally, suggesting a suppression of AGN triggering in denser environment. In order to investigate the origin of the X-ray luminosity dependence, we are also investigating the dependence of clustering on the black hole mass and the Eddington ratio, we also present the results of this investigation.

scholarly journals GALAXY CLUSTERING TOPOLOGY IN THE SLOAN DIGITAL SKY SURVEY MAIN GALAXY SAMPLE: A TEST FOR GALAXY FORMATION MODELS

2010 ◽  
Vol 190 (1) ◽  
pp. 181-202 ◽  
Author(s):  
Yun-Young Choi ◽  
Changbom Park ◽  
Juhan Kim ◽  
J. Richard Gott ◽  
David H. Weinberg ◽  
...  
Keyword(s):  
Galaxy Formation ◽  
Sloan Digital Sky Survey ◽  
Galaxy Clustering ◽  
Main Galaxy ◽  
Sky Survey ◽  
Galaxy Sample

The Search for Galaxy Clustering around a Quasar Pair at z =4.25 Found in the Sloan Digital Sky Survey

2004 ◽  
Vol 603 (2) ◽  
pp. L65-L68 ◽  
Author(s):  
Masataka Fukugita ◽  
Osamu Nakamura ◽  
Donald P. Schneider ◽  
Mamoru Doi ◽  
Nobunari Kashikawa
Keyword(s):  
Sloan Digital Sky Survey ◽  
Galaxy Clustering ◽  
Sky Survey

scholarly journals The Milky Way’s total satellite population and constraining the mass of the warm dark matter particle

2018 ◽  
Vol 14 (S344) ◽  
pp. 109-113 ◽  
Author(s):  
Oliver Newton ◽  
Marius Cautun ◽  
Adrian Jenkins ◽  
Carlos S. Frenk ◽  
John C. Helly
Keyword(s):  
Dark Matter ◽  
Dark Matter Particle ◽  
Statistical Error ◽  
Sloan Digital Sky Survey ◽  
Dark Energy Survey ◽  
Satellite Galaxy ◽  
Sky Survey ◽  
Galaxy Luminosity Function ◽  
Energy Survey ◽  
Rule Out

AbstractThe Milky Way’s (MW) satellite population is a powerful probe of warm dark matter (WDM) models as the abundance of small substructures is very sensitive to the properties of the WDM particle. However, only a partial census of the MW’s complement of satellite galaxies exists because surveys of the MW’s close environs are incomplete both in depth and in sky coverage. We present a new Bayesian analysis that combines the sample of satellites recently discovered by the Dark Energy Survey (DES) with those found in the Sloan Digital Sky Survey (SDSS) to estimate the total satellite galaxy luminosity function down to Mv = 0. We find that there should be at least $124_{ - 27}^{ + 40}$ (68% CL, statistical error) satellites as bright or brighter than Mv = 0 within 300 kpc of the Sun, with only a weak dependence on MW halo mass. When it comes online the Large Synoptic Survey Telescope should detect approximately half of this population. We also show that WDM models infer the same number of satellites as in ΛCDM, which will allow us to rule out those models that produce insufficient substructure to be viable.

scholarly journals KiDS+GAMA: Intrinsic alignment model constraints for current and future weak lensing cosmology

2019 ◽  
Vol 624 ◽  
pp. A30 ◽  
Author(s):  
Harry Johnston ◽  
Christos Georgiou ◽  
Benjamin Joachimi ◽  
Henk Hoekstra ◽  
Nora Elisa Chisari ◽  
...  
Keyword(s):  
Sloan Digital Sky Survey ◽  
Weak Lensing ◽  
Satellite Galaxy ◽  
Sky Survey ◽  
The Galaxy ◽  
Resolution Imaging ◽  
Cosmic Shear ◽  
Linear Alignment ◽  
Red Galaxies ◽  
Blue Galaxy

We directly constrain the non-linear alignment (NLA) model of intrinsic galaxy alignments, analysing the most representative and complete flux-limited sample of spectroscopic galaxies available for cosmic shear surveys. We measure the projected galaxy position-intrinsic shear correlations and the projected galaxy clustering signal using high-resolution imaging from the Kilo Degree Survey (KiDS) overlapping with the GAMA spectroscopic survey, and data from the Sloan Digital Sky Survey. Separating samples by colour, we make no significant detection of blue galaxy alignments, constraining the blue galaxy NLA amplitude AIAB = 0.21−0.36+0.37 to be consistent with zero. We make robust detections (∼9σ) for red galaxies, with AIAR = 3.18−0.46+0.47, corresponding to a net radial alignment with the galaxy density field, and we find no evidence for any scaling of alignments with galaxy luminosity. We provide informative priors for current and future weak lensing surveys, an improvement over de facto wide priors that allow for unrealistic levels of intrinsic alignment contamination. For a colour-split cosmic shear analysis of the final KiDS survey area, we forecast that our priors will improve the constraining power on S8 and the dark energy equation of state w0, by up to 62% and 51%, respectively. Our results indicate, however, that the modelling of red/blue-split galaxy alignments may be insufficient to describe samples with variable central/satellite galaxy fractions.

scholarly journals Updated results on the galaxy–halo connection from satellite kinematics in SDSS

2019 ◽  
Vol 487 (3) ◽  
pp. 3112-3129 ◽  
Author(s):  
Johannes U Lange ◽  
Frank C van den Bosch ◽  
Andrew R Zentner ◽  
Kuan Wang ◽  
Antonio S Villarreal
Keyword(s):  
Dark Matter ◽  
Radial Profile ◽  
Sloan Digital Sky Survey ◽  
Galaxy Clustering ◽  
Sky Survey ◽  
The Galaxy ◽  
Blue Galaxies ◽  
Galaxy Halo ◽  
Satellite Galaxies ◽  
The Relationship

ABSTRACT We present new results on the relationship between central galaxies and dark matter haloes inferred from observations of galaxy abundances and satellite kinematics in the Sloan Digital Sky Survey (SDSS) DR7. We employ an updated analysis framework that includes detailed mock catalogues to model observational effects in SDSS. Our results constrain the colour-dependent conditional luminosity function of dark matter haloes, as well as the radial profile of satellite galaxies. Confirming previous results, we find that red central galaxies live in more massive haloes than blue galaxies at a fixed luminosity. Additionally, our results suggest that satellite galaxies have a radial profile less centrally concentrated than dark matter but not as cored as resolved subhaloes in dark-matter-only simulations. Compared to previous works using satellite kinematics by More et al., we find much more competitive constraints on the galaxy–halo connection, on par with those derived from a combination of galaxy clustering and galaxy–galaxy lensing. This improvement stems from also modelling the abundance of galaxies as well as a larger sample size and more realistic observational uncertainties. We compare our results on the galaxy–halo connection to other studies using galaxy clustering and group catalogues, showing a reasonable agreement between these different techniques. We discuss future applications of satellite kinematics in the context of constraining cosmology and the relationship between galaxies and dark matter haloes.

scholarly journals Basic properties of galaxy clustering in the light of recent results from the Sloan Digital Sky Survey

2005 ◽  
Vol 443 (1) ◽  
pp. 11-16 ◽  
Author(s):  
M. Joyce ◽  
F. Sylos Labini ◽  
A. Gabrielli ◽  
M. Montuori ◽  
L. Pietronero
Keyword(s):  
Sloan Digital Sky Survey ◽  
Galaxy Clustering ◽  
Basic Properties ◽  
Sky Survey

scholarly journals BRIGHTEST SATELLITE GALAXY ALIGNMENT OF SLOAN DIGITAL SKY SURVEY GALAXY GROUPS

2013 ◽  
Vol 768 (1) ◽  
pp. 20 ◽  
Author(s):  
Zhigang Li ◽  
Yougang Wang ◽  
Xiaohu Yang ◽  
Xuelei Chen ◽  
Lizhi Xie ◽  
...  
Keyword(s):  
Sloan Digital Sky Survey ◽  
Galaxy Groups ◽  
Satellite Galaxy ◽  
Sky Survey

scholarly journals Calculation of velocity dispersion of the nearby galaxies using different stellar template libraries

2010 ◽  
pp. 57-69
Author(s):  
Ana Lalovic
Keyword(s):  
Reasonable Agreement ◽  
Velocity Dispersion ◽  
Signal To Noise Ratio ◽  
Sloan Digital Sky Survey ◽  
Signal To Noise ◽  
Method Of Calculation ◽  
Sky Survey ◽  
Best Fitting ◽  
Nearby Galaxies ◽  
Spectral Libraries

We present the central velocity dispersion measurements of the nearby galaxies from the Sloan Digital Sky Survey (SDSS). Using the sample from the paper by Ho et al. 2009, we have selected 23 galaxies for which we calculate the velocity dispersion. We have used the Penalized Pixel-Fitting code (Cappellari and Emsellem2004) to measure the velocity dispersion throughout the four chosen spectral regions: (3800,4568)?A, (4568,5336)?A, (5336,6104) and (6104,6872)?A. In all these regions, we have separately calculated dispersions and corresponding errors. We found that the measured values may vary with the change of spectral region, but, if weighted properly with the measure of the goodness of the fit, the final results will be shifted coloser to those for the best fitting regions. We have also tested how the use of different spectral libraries (Miles, Valdes and Elodie databases) influences measurements and we showed that they do not affect measurements much. However, Elodie stellar library introduces the smallest errors in the velocity dispersion and it is the most stable throughout all four spectral regions. For these reasons it should be used preferentially when dealing with the SDSS spectra. We compare the results with the above mentioned paper and find a reasonable agreement. The agreement with the dispersions available in the HyperLeda database is very poor. The best agreement is obtained with SDSS measurements. We believe that our measurements are useful since SDSS velocity dispersions measurements are not available for many galaxies and the method of calculation of the velocity dispersion outlined in this work enables calculation of velocity dispersion for any galaxy. Of course, spectra with signal-to-noise ratio below 20 should be taken with caution.

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