Open AccessThe effect of large‐scale structure on the SDSS galaxy three‐point correlation function
Author(s) -
Nichol R. C.,
Sheth R. K.,
Suto Y.,
Gray A. J.,
Kayo I.,
Wechsler R. H.,
Marin F.,
Kulkarni G.,
Blanton M.,
Connolly A. J.,
Gardner J. P.,
Jain B.,
Miller C. J.,
Moore A. W.,
Pope A.,
Pun J.,
Schneider D.,
Schneider J.,
Szalay A.,
Szapudi I.,
Zehavi I.,
Bahcall N. A.,
Csabai I.,
Brinkmann J.
Publication year - 2006
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2006.10239.x
Subject(s) - physics , astrophysics , galaxy , correlation function (quantum field theory) , supercluster (genetic) , redshift , sky , field galaxy , luminosity function , redshift survey , luminosity , universe , astronomy , biochemistry , chemistry , phylogenetics , optoelectronics , dielectric , gene
We present measurements of the normalized redshift‐space three‐point correlation function (3PCF) ( Q z ) of galaxies from the Sloan Digital Sky Survey (SDSS) main galaxy sample. These measurements were possible because of a fast new N ‐point correlation function algorithm (called npt ) based on multiresolutional k‐d trees. We have applied npt to both a volume‐limited (36 738 galaxies with 0.05 ≤ z ≤ 0.095 and −23 ≤ M 0.0 r ≤−20.5 ) and magnitude‐limited sample (134 741 galaxies over 0.05 ≤ z ≤ 0.17 and ∼ M *± 1.5 ) of SDSS galaxies, and find consistent results between the two samples, thus confirming the weak luminosity dependence of Q z recently seen by other authors. We compare our results to other Q z measurements in the literature and find it to be consistent within the full jackknife error estimates. However, we find these errors are significantly increased by the presence of the ‘Sloan Great Wall’ (at z ∼0.08) within these two SDSS data sets, which changes the 3PCF by 70 per cent on large scales ( s ≥ 10 h −1 Mpc) . If we exclude this supercluster, our observed Q z is in better agreement with that obtained from the 2‐degree Field Galaxy Redshift Survey (2dFGRS) by other authors, thus demonstrating the sensitivity of these higher order correlation functions to large‐scale structures in the Universe. This analysis highlights that the SDSS data sets used here are not ‘fair samples’ of the Universe for the estimation of higher order clustering statistics and larger volumes are required. We study the shape dependence of Q z ( s , q , θ) as one expects this measurement to depend on scale if the large‐scale structure in the Universe has grown via gravitational instability from Gaussian initial conditions. On small scales ( s ≤ 6 h −1 Mpc) , we see some evidence for shape dependence in Q z , but at present our measurements are consistent with a constant within the errors ( Q z ≃ 0.75 ± 0.05) . On scales >10 h −1 Mpc , we see considerable shape dependence in Q z . However, larger samples are required to improve the statistical significance of these measurements on all scales.