FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W3099875550> ?p ?o ?g. }

• W3099875550 endingPage "620" @default.
• W3099875550 startingPage "613" @default.
• W3099875550 abstract "We use the projected correlation function wp(rp) of a volume-limited subsample of the Sloan Digital Sky Survey (SDSS) main galaxy-redshift catalog to measure the halo occupation distribution (HOD) of the galaxies of the sample. Simultaneously, we allow the cosmology to vary within cosmological constraints imposed by cosmic microwave background experiments in a ΛCDM model. We find that combining wp(rp) for this sample alone with observations by the Wilkinson Microwave Anisotropy Probe (WMAP), Arcminute Cosmology Bolometer Array Receiver (ACBAR), Cosmic Background Imager (CBI), and Very Small Array (VSA) can provide one of the most precise techniques available to measure cosmological parameters. For a minimal, flat, six-parameter ΛCDM model with an HOD with three free parameters, we find Ωm = 0.278, σ8 = 0.812, and H0 = 69.8 km s-1 Mpc-1; these errors are significantly smaller than from cosmic microwave background (CMB) alone and similar to those obtained by combining CMB with the large-scale galaxy power spectrum assuming scale-independent bias. The corresponding HOD parameters describing the minimum halo mass and the normalization and cutoff of the satellite mean occupation are Mmin = (3.03) × 1012 h-1 M☉, M1 = (4.58) × 1013 h-1 M☉, and κ = 4.44. These HOD parameters thus have small fractional uncertainty when cosmological parameters are allowed to vary within the range permitted by the data. When more parameters are added to the HOD model, the error bars on the HOD parameters increase because of degeneracies, but the error bars on the cosmological parameters do not increase greatly. Similar modeling for other galaxy samples could reduce the statistical errors on these results, while more thorough investigations of the cosmology dependence of nonlinear halo bias and halo mass functions are needed to eliminate remaining systematic uncertainties, which may be comparable to statistical uncertainties." @default.
• W3099875550 created "2020-11-23" @default.
• W3099875550 creator A5008915976 @default.
• W3099875550 creator A5021421082 @default.
• W3099875550 creator A5030308731 @default.
• W3099875550 creator A5032155044 @default.
• W3099875550 creator A5036500718 @default.
• W3099875550 creator A5052786955 @default.
• W3099875550 creator A5055630635 @default.
• W3099875550 creator A5070394199 @default.
• W3099875550 creator A5071423709 @default.
• W3099875550 creator A5091405403 @default.
• W3099875550 creator A5091601455 @default.
• W3099875550 date "2005-06-01" @default.
• W3099875550 modified "2023-09-24" @default.
• W3099875550 title "Cosmology and the Halo Occupation Distribution from Small‐Scale Galaxy Clustering in the Sloan Digital Sky Survey" @default.
• W3099875550 cites W1506722212 @default.
• W3099875550 cites W1847269195 @default.
• W3099875550 cites W1944901286 @default.
• W3099875550 cites W1964357829 @default.
• W3099875550 cites W1965779302 @default.
• W3099875550 cites W1967936658 @default.
• W3099875550 cites W1969935241 @default.
• W3099875550 cites W1976620664 @default.
• W3099875550 cites W1978875836 @default.
• W3099875550 cites W1979742375 @default.
• W3099875550 cites W1982533357 @default.
• W3099875550 cites W1982576080 @default.
• W3099875550 cites W1983645991 @default.
• W3099875550 cites W1986264263 @default.
• W3099875550 cites W1994900330 @default.
• W3099875550 cites W2011193290 @default.
• W3099875550 cites W2018719255 @default.
• W3099875550 cites W2019267312 @default.
• W3099875550 cites W2023393371 @default.
• W3099875550 cites W2026354508 @default.
• W3099875550 cites W2026619221 @default.
• W3099875550 cites W2032327414 @default.
• W3099875550 cites W2035000458 @default.
• W3099875550 cites W2035399222 @default.
• W3099875550 cites W2037502800 @default.
• W3099875550 cites W2045377202 @default.
• W3099875550 cites W2046341417 @default.
• W3099875550 cites W2049137639 @default.
• W3099875550 cites W2059699043 @default.
• W3099875550 cites W2061899254 @default.
• W3099875550 cites W2064377583 @default.
• W3099875550 cites W2097707314 @default.
• W3099875550 cites W2101568531 @default.
• W3099875550 cites W2103185872 @default.
• W3099875550 cites W2103809124 @default.
• W3099875550 cites W2106871347 @default.
• W3099875550 cites W2109510044 @default.
• W3099875550 cites W2118265220 @default.
• W3099875550 cites W2121862896 @default.
• W3099875550 cites W2129489826 @default.
• W3099875550 cites W2130908251 @default.
• W3099875550 cites W2132575702 @default.
• W3099875550 cites W2133218664 @default.
• W3099875550 cites W2133543752 @default.
• W3099875550 cites W2134712793 @default.
• W3099875550 cites W2141138389 @default.
• W3099875550 cites W2142635246 @default.
• W3099875550 cites W2150195330 @default.
• W3099875550 cites W2150331774 @default.
• W3099875550 cites W2153208487 @default.
• W3099875550 cites W2153811626 @default.
• W3099875550 cites W2157917411 @default.
• W3099875550 cites W2158236716 @default.
• W3099875550 cites W2168175751 @default.
• W3099875550 cites W2593311270 @default.
• W3099875550 cites W2951034677 @default.
• W3099875550 cites W3099676335 @default.
• W3099875550 cites W3100336792 @default.
• W3099875550 cites W3100429683 @default.
• W3099875550 cites W3100897521 @default.
• W3099875550 cites W3101136340 @default.
• W3099875550 cites W3101247804 @default.
• W3099875550 cites W3101610418 @default.
• W3099875550 cites W3102483686 @default.
• W3099875550 cites W3103838041 @default.
• W3099875550 cites W3103877238 @default.
• W3099875550 cites W3104266932 @default.
• W3099875550 cites W3104639138 @default.
• W3099875550 cites W3106014062 @default.
• W3099875550 cites W3106072945 @default.
• W3099875550 cites W3106449272 @default.
• W3099875550 cites W4292310541 @default.
• W3099875550 cites W2080376038 @default.
• W3099875550 doi "https://doi.org/10.1086/429685" @default.
• W3099875550 hasPublicationYear "2005" @default.
• W3099875550 type Work @default.
• W3099875550 sameAs 3099875550 @default.
• W3099875550 citedByCount "84" @default.
• W3099875550 countsByYear W30998755502012 @default.
• W3099875550 countsByYear W30998755502013 @default.
• W3099875550 countsByYear W30998755502015 @default.
• W3099875550 countsByYear W30998755502016 @default.

• next