The 2dF Galaxy Redshift Survey: The dependence of galaxy clustering on luminosity and spectral type

Abstract

We investigate the dependence of galaxy clustering on luminosity and spectral type using the 2dF Galaxy Redshift Survey (2dFGRS). Spectral types are assigned using the principal component analysis of Madgwick et al. We divide the sample into two broad spectral classes: galaxies with strong emission lines (`late-types'), and more quiescent galaxies (`early-types'). We measure the clustering in real space, free from any distortion of the clustering pattern due to peculiar velocities, for a series of volume-limited samples. The projected correlation functions of both spectral types are well described by a power law for transverse separations in the range 2 < (sigma/Mpc/h) < 15, with a marginally steeper slope for early-types than late-types. Both early and late types have approximately the same dependence of clustering strength on luminosity, with the clustering amplitude increasing by a factor of ~2.5 between L* and 4 L*. At all luminosities, however, the correlation function amplitude for the early-types is ~50% higher than that of the late-types. These results support the view that luminosity, and not type, is the dominant factor in determining how the clustering strength of the whole galaxy population varies with luminosity.

accepted by MNRAS after minor revision. 13 pages, 10 figures

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• Anisotropies in the redshift-space correlations of galaxy groups and clusters I: Simulated catalogues
• Dwarf Galaxy Clustering and Missing Satellites
• Galaxy clustering using photometric redshifts
• Joint constraints on galaxy bias and ${\sigma }_8$ through the N-pdf of the galaxy number density
• Nature and Environment of Very Luminous Galaxies
• CFHTLenS: Galaxy bias as function of scale, stellar mass, and colour. Conflicts with predictions by semi-analytic models
• What is the optimal way to measure the galaxy power spectrum?
• Measuring the growth of structure by matching dark matter haloes to galaxies with VIPERS and SDSS
• Estimating lifetimes of uv-selected massive galaxies at $0.5\le z\le 2.5$ in the cosmos/ultravista field through clustering analyses
• A Large Massive Quiescent Galaxy Sample at z~1.2
• Galaxy and Mass Assembly (GAMA): Mid-infrared properties as tracers of galaxy environment
• Practical Statistics for the Voids Between Galaxies
• The Redshift-Space Two Point Correlation Function of ELAIS-S1 Galaxies
• The ergodicity bias in the observed galaxy distribution
• Spatial clustering in the ESO-Sculptor Survey: two-point correlation functions by galaxy type at redshifts 0.1 - 0.5
• Toward accurate measurement of property-dependent galaxy clustering I. Comparison of the Vmax method and the "shuffled" method
• Toward accurate measurement of property-dependent galaxy clustering: II. Tests of the smoothed density-corrected $V_{\max }$ method
• Luminosity segregation versus fractal scaling in the galaxy distribution
• Particle Physics in the Sky and Astrophysics Underground: Connecting the Universe's Largest and Smallest Scales
• Clustering Evolution Between z=1 And Today
• Morphological Transformation and Star Formation Quenching of Massive Galaxies at 0.5 < z < 2.5 in 3D-HST/CANDELS
• The spatial clustering of radio sources in NVSS and FIRST; implications for galaxy clustering evolution
• Colour Dependence of the Distribution of IRAS Galaxies revealed by Multifractal Measures