The spatial correlation function of IRAS galaxies on small and intermediate scales

Saunders, W.; Rowan-Robinson, M.; Lawrence, Andy

doi:10.1093/mnras/258.1.134

Cited by 140 publications

(179 citation statements)

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“…For the IRAS galaxies we have two estimates of the number density fluctuations: one from the QDOT survey [43] b I σ non−linear (8h −1 Mpc) = 0.69 ± 0.09 (3.6) which is in perfect agreement with the estimate from the Berkeley survey [44] …”

Section: σ(8h −1 Mpc)supporting

confidence: 74%

Simple model of large scale structure formation

Schaefer

Shafi

1994

Phys. Rev. D

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We explore constraints on inflationary models employing data on large scale structure mainly from COBE temperature anisotropies and IRAS selected galaxy surveys, taking care not to apply linear perturbation theory to data in the non-linear regime. In models where the tensor contribution to the COBE signal is negligible, we find the spectral index of density fluctuations n must exceed 0.7. Furthermore the COBE signal cannot be dominated by the tensor component, implying n > 0.85 in such models. The data favors cold plus hot dark matter models with n close to unity and Ω HDM ∼ 0.20 − 0.35. We present realistic grand unified theories, including supersymmetric versions, which produce inflation with these properties.98.65 Dx,98.80 Cq,12.10 Dm

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Section: σ(8h −1 Mpc)supporting

confidence: 74%

Simple model of large scale structure formation

Schaefer

Shafi

1994

Phys. Rev. D

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“…The slope of the correlation function, c, becomes steeper with increasingly red color. Both of these e †ects are known at lower redshift as morphological type or emission/absorption line galaxy correlations, although the large range of correlation amplitudes we Ðnd is not so readily apparent at low redshift (Davis & Geller 1976 ;Saunders, Rowan-Robinson, & Lawrence 1992 ;Fisher et al 1994 ;Guzzo et al 1997 ;Willmer, da Costa, & Pellegrini 1998 ;Loveday, Tresse, & Maddox 1999). The most relevant measure of correlation amplitude in a situation where the c vary systematically is to show the correlation length normalized to a Ðxed c, here chosen to be c \ 1.8.…”

Section: Introductionmentioning

confidence: 95%

Environment and Galaxy Evolution at Intermediate Redshift in the CNOC2 Survey

Carlberg

Yee

Morris

et al. 2001

ApJ

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The systematic variation of galaxy colors and types with clustering environment could either be the result of local conditions at formation or subsequent environmental e †ects as larger scale structures draw together galaxies whose stellar mass is largely in place. Below redshift 0.7 galaxy luminosities (k-corrected and evolution compensated) are relatively invariant, whereas galaxy star formation rates, as reÑected in their colors, are a "" transient ÏÏ property that have a wide range for a given luminosity. The relations between these galaxy properties and the clustering properties are key statistics for understanding the forces driving late-time galaxy evolution. At z D 0.4 the comoving galaxy correlation length, mear 0 , sured in the CNOC2 sample is strongly color dependent, rising from 2 h~1 Mpc to nearly 10 h~1 Mpc as the volume-limited subsamples range from blue to red. The luminosity dependence of at z D 0.4 is r 0 weak below in the R band, although there is an upturn at high luminosity, where its interpretation L * depends on separating it from the relation. In the B band there is a slow, smooth increase of r 0 -color r 0 with luminosity, at least partially related to the color dependence. Study of the evolution of galaxies within groups, which create much of the strongly nonlinear correlation signal, allows a physical investigation of the source of these relations. The dominant e †ect of the group environment on star formation is seen in the radial gradient of the mean galaxy colors, which on the average become redder than the Ðeld toward the group centers. The color di †erentiation begins around the dynamical radius of virialization of the groups. The redder-than-Ðeld trend applies to groups with a line-of-sight velocity dispersion, km s~1. There is an indication, somewhat statistically insecure, that the high-luminosity galp 1 [ 150 axies in groups with km s~1 become bluer toward the group center. Monte Carlo orbit intep 1 \ 125 grations initiated at the measured positions and velocities show that the rate of galaxy merging in the km s~1 groups is very low, whereas for km s~1 about 25% of the galaxies will merge p 1 [ 150 p 1 \ 150 in 0.5 Gyr. We conclude that the higher velocity dispersion groups largely act to suppress star formation relative to the less clustered Ðeld, leading to "" embalmed ÏÏ galaxies. On the other hand, the low velocity dispersion groups are prime sites of both strong merging and enhanced star formation that leads to the formation of some new massive galaxies at intermediate redshifts. The tidal Ðelds within the groups appear to be a strong candidate for the physical source of the reduction of star formation in group galaxies relative to Ðeld. Tides operate e †ectively at all velocity dispersions to remove gas-rich companions and low-density gas in galactic halos. We Ðnd a close resemblance of the color-dependent galaxy luminosity function evolution in the Ðeld and groups, suggesting that the clustering-dependent star formation reduction mechanism is important for the e...

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“…The KOS survey consists of redshifts for 164 field galaxies brighter than J = 15.0 in the north and south galactic caps. The IRAS redshift survey represents results from both the S 60 ≥ 0.6 Jy (Saunders et al 1992) and S 60 ≥ 1.2…”

Section: Discussionmentioning

confidence: 99%