Eisenstein DJ, Zaldarriaga M.
Correlations in the Spatial Power Spectra Inferred from Angular Clustering: Methods and Application to the Automated Plate Measuring Survey. The Astrophysical Journal. 2001;546 :2-19.
Publisher's VersionAbstractWe reconsider the inference of spatial power spectra from angularclustering data and show how to include correlations in both the angularcorrelation function and the spatial power spectrum. Inclusion of thefull covariance matrices loosens the constraints on large-scalestructure inferred from the Automated Plate Measuring (APM) survey byover a factor of 2. We present a new inversion technique based onsingular-value decomposition that allows one to propagate the covariancematrix on the angular correlation function through to that of thespatial power spectrum and to reconstruct smooth power spectra withoutunderestimating the errors. Within a parameter space of the cold darkmatter (CDM) shape Γ and the amplitude σ8, wefind that the angular correlations in the APM survey constrain Γ
Knox L, Cooray A, Eisenstein D, Haiman Z.
Probing Early Structure Formation with Far-Infrared Background Correlations. The Astrophysical Journal. 2001;550 :7-20.
Publisher's VersionAbstractThe large-scale structure of high-redshift galaxies produces correlatedanisotropy in the far-infrared background (FIRB). In regions of the skywhere the thermal emission from Galactic dust is well below average,these high-redshift correlations may be the most significant source ofangular fluctuation power over a wide range of angular scales, from ~7'to ~3°, and frequencies, from ~400 to ~1000 GHz. The strength ofthis signal should allow detailed studies of the statistics of the FIRBfluctuations, including the shape of the angular power spectrum at agiven frequency and the degree of coherence between FIRB maps atdifferent frequencies. The FIRB correlations depend on and henceconstrain the redshift-dependent spectral energy distributions, numbercounts, and clustering bias of the galaxies and active nuclei thatcontribute to the background. We quantify the accuracy to which Planckand a newly proposed balloon-borne mission, Explorer of Diffuse GalacticEmissions, could constrain models of the high-redshift universe throughthe measurement of FIRB fluctuations. We conclude that the average bias
Blanton MR, Dalcanton J, Eisenstein D, Loveday J, Strauss MA, SubbaRao M, Weinberg DH, Anderson, John E. J, Annis J, Bahcall NA, et al. The Luminosity Function of Galaxies in SDSS Commissioning Data. The Astronomical Journal. 2001;121 :2358-2380.
Publisher's VersionAbstractIn the course of its commissioning observations, the Sloan Digital SkySurvey (SDSS) has produced one of the largest redshift samples ofgalaxies selected from CCD images. Using 11,275 galaxies complete tor*=17.6 over 140 deg2, we compute the luminosityfunction of galaxies in the r* band over a range-23r*<-16 (for h=1). The result iswell-described by a Schechter function with parametersφ*=(1.46+/-0.12)×10-2 h3Mpc-3, M*=-20.83+/-0.03, and α=-1.20+/-0.03.The implied luminosity density in r* isj~(2.6+/-0.3)×108h Lsolar Mpc-3.We find that the surface brightness selection threshold has a negligibleimpact for Mr*<-18. Using subsets of the data,we measure the luminosity function in the u*, g*,i*, and z* bands as well; the slope at lowluminosities ranges from α=-1.35 to α=-1.2. We measure thebivariate distribution of r* luminosity with half-lightsurface brightness, intrinsic g*-r* color, andmorphology. In agreement with previous studies, we find that highsurface brightness, red, highly concentrated galaxies are on averagemore luminous than low surface brightness, blue, less concentratedgalaxies. An important feature of the SDSS luminosity function is theuse of Petrosian magnitudes, which measure a constant fraction of agalaxy's total light regardless of the amplitude of its surfacebrightness profile. If we synthesize results for RGKC band orbj band using these Petrosian magnitudes, we obtainluminosity densities 2 times that found by the Las Campanas RedshiftSurvey in RGKC and 1.4 times that found by the Two DegreeField Galaxy Redshift Survey in bj. However, we are able toreproduce the luminosity functions obtained by these surveys if we alsomimic their isophotal limits for defining galaxy magnitudes, which areshallower and more redshift dependent than the Petrosian magnitudes usedby the SDSS. Based on observations obtained with the Sloan Digital SkySurvey.
Eisenstein DJ, Annis J, Gunn JE, Szalay AS, Connolly AJ, Nichol RC, Bahcall NA, Bernardi M, Burles S, Castander FJ, et al. Spectroscopic Target Selection for the Sloan Digital Sky Survey: The Luminous Red Galaxy Sample. The Astronomical Journal. 2001;122 :2267-2280.
Publisher's VersionAbstractWe describe the target selection and resulting properties of aspectroscopic sample of luminous red galaxies (LRGs) from the imagingdata of the Sloan Digital Sky Survey (SDSS). These galaxies are selectedon the basis of color and magnitude to yield a sample of luminousintrinsically red galaxies that extends fainter and farther than themain flux-limited portion of the SDSS galaxy spectroscopic sample. Thesample is designed to impose a passively evolving luminosity andrest-frame color cut to a redshift of 0.38. Additional, yet moreluminous red galaxies are included to a redshift of ~0.5. Approximately12 of these galaxies per square degree are targeted for spectroscopy, sothe sample will number over 100,000 with the full survey. SDSScommissioning data indicate that the algorithm efficiently selectsluminous (M*g~-21.4) red galaxies, that thespectroscopic success rate is very high, and that the resulting set ofgalaxies is approximately volume limited out to z=0.38. When the SDSS iscomplete, the LRG spectroscopic sample will fill over 1 h-3Gpc3 with an approximately homogeneous population of galaxiesand will therefore be well suited to studies of large-scale structureand clusters out to z=0.5.