The Power Spectrum of Galaxy Clustering in the Las Campanas Redshift Survey

We present the power spectrum P (k), over scales = 2 =k = 5 400 h 1 Mpc, for a magnitude-limited sample of 19276 Las Campanas Redshift Survey (LCRS) galaxies, with average redshift z 0:1. The LCRS P (k) may be approximated as / k 1:8 for small scales = 5 30 h 1 Mpc, changing to / k 1 1 for large scales 200 400 h 1 Mpc. The overall amplitude corresponds to 8 = 1 in redshift space. We also compare our results to those of several other redshift surveys. For < 100 h 1 Mpc, the LCRS P (k) is roughly similar in shape to the P (k) of other surveys, but with an amplitude di ering from some of the other samples, possibly because of inherent clustering di erences among di erent types of galaxies. For > 100 h 1 Mpc, the LCRS results are consistent with those of other surveys, given the large errors among all the surveys on these scales. 1 The Las Campanas Redshift Survey Data The Las Campanas Redshift Survey (LCRS) contains 26400 galaxies, with an average redshift z 0:1, distributed over 6 1:5 80 slices, 3 each in the North and South galactic caps. The survey galaxies were selected from an R-band CCD photometric catalog, and were chosen using nominal isophotal magnitude limits 16:0 < R < 17:3 for the initial 20% of the data and 15:0 < R < 17:7 for the remainder. Spectroscopy was carried out using the multi-object ber-optic spectrograph on the Las Campanas 2.5-m telescope. Additional survey details may be found in [5] and [6]. Figure 1 shows the survey's galaxy distribution, revealing a rich pattern of laments, clusters, and voids. South 13885 galaxies North 12545 galaxies cz (1000 km/s) RA Dec 10 20 30 40 50 60 -45 -42 -39 21 h 22 h 23 h 0 h 1 h 2 h 3 h 4 h 10 20 30 40 50 60 -12 o -6 o -3 o 10 h 11 h 12 h 13 h 14 h 15 h Figure 1. The distribution of galaxies in the LCRS in redshift and right ascension. The distribution of the same galaxies on the sky, in right ascension and declination, is also shown in the outer circular section of the gure. po w er P ( h -1 M pc ) 3 wavenumber k (h Mpc) wavelength λ = 2π / k (h -1 Mpc) 1000 100 10 .01 .1 1 10