Constraints on Cosmological Parameters from the Lyα Forest Power Spectrum and<i>COBE</i>DMR

Phillips, John; Weinberg, David H.; Croft, Rupert A. C.; Hernquist, Lars; Katz, Neal

doi:10.1086/322369

Cited by 36 publications

(45 citation statements)

References 61 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…1, the LFs are measured for cosmological parameters Ω m = 1.0 and Ω Λ = 0.0. Because the faint number counts Table 1. which we use below to constrain the ESS evolution rate are sensitive to the cosmological parameters, we have converted these values to Ω m = 0.3 and Ω Λ = 0.7, the currently favored parameters (Riess et al 1998;Perlmutter et al 1999;Phillips et al 2001;Tonry et al 2003). Again, rather than re-running the composite fits, we apply the empirical corrections derived by de Lapparent (2003), as follows.…”

Section: The Shape Of the Ess Luminosity Functionsmentioning

confidence: 99%

The ESO-Sculptor Survey: Evolution of late-type galaxies at redshifts 0.1–0.5

Lapparent

Arnouts

Galaz

et al. 2004

A&A

View full text Add to dashboard Cite

Abstract. Using the Gaussian+Schechter composite luminosity functions measured from the ESO-Sculptor Survey (de Lapparent et al. 2003, A&A, 404, 831) and assuming that these functions do not evolve with redshift out to z ∼ 1, we obtain evidence for evolution in the late spectral class containing late-type Spiral (Sc+Sd) and dwarf Irregular (dI) galaxies. There are indications that the Sc+Sd galaxies are the evolving population, but we cannot exclude that the dI galaxies also undergo some evolution. This evolution is detected as an increase of the Sc+Sd+dI galaxy density which can be modeled as2 using the currently favored cosmological parameters Ω m = 0.3 and Ω Λ = 0.7; the uncertainty in the linear and power-law evolution rates is of the order of unity. For Ω m = 1.0 and Ω Λ = 0.0, the linear and power-law evolution rates are ∼4 ± 1 and ∼2.5 ± 1 respectively. Both models yield a good match to the ESS BVR c redshift distributions to 21−22 mag and to the number-counts to 23−23.5 mag , which probe the galaxy distribution to redshifts z ∼ 0.5 and z ∼ 1.0 respectively. The present analysis shows the usefulness of the joint use of the magnitude and redshift distributions for studying galaxy evolution. It also illustrates how Gaussian+Schechter composite luminosity functions provide more robust constraints on the evolution rate than pure Schechter luminosity functions, thus emphasizing the importance of performing realistic parameterizations of the luminosity functions for studying galaxy evolution. The detected density evolution indicates that mergers could play a significant role in the evolution of late-type Spiral and dwarf Irregular galaxies. However, the ESO-Sculptor density increase with redshift could also be caused by a ∼1 mag brightening of the Sc+Sd+dI galaxies at z ∼ 0.5 and a ∼ 1.5−2.0 mag brightening at z ∼ 1, which is compatible with the expected passive brightening of Sc galaxies at these redshifts. Distinguishing between luminosity and density evolution is a major difficulty as these produce the same effect on the redshift and magnitude distributions. The detected evolution rate of the ESO-Sculptor Sc+Sd+dI galaxies is nevertheless within the range of measured values from the other existing analyses, whether they provide evidence for density or luminosity evolution.

show abstract

Section: The Shape Of the Ess Luminosity Functionsmentioning

confidence: 99%

The ESO-Sculptor Survey: Evolution of late-type galaxies at redshifts 0.1–0.5

Lapparent

Arnouts

Galaz

et al. 2004

A&A

View full text Add to dashboard Cite

show abstract

“…Whether such lensing is common or rare depends on exactly what you are asking. Significant amplification of flux received from sources at large redshift is common (Wyithe & Loeb 2002), while actually seeing two or more images at any redshift is rare (Phillips et al 2001), indeed rare to the point where it butts its head against values of the cosmological constant as large as the ones favored in § 12. Similarly, some rapid variability is caused by microlensing (stars in an intervening galaxy passing through the line of sight), but most is not (Chartas et al 2002;Trevese & Vagnetti 2002).…”

Section: Big Brother Is Watching (Or At Least Radiating At) You: Actimentioning

confidence: 99%

Astrophysics in 2002

Trimble

Aschwanden

2003

PUBL ASTRON SOC PAC

View full text Add to dashboard Cite

ABSTRACT. This has been the Year of the Baryon. Some low temperature ones were seen at high redshift, some high temperature ones were seen at low redshift, and some cooling ones were (probably) reheated. Astronomers saw the back of the Sun (which is also made of baryons), a possible solution to the problem of ejection of material by Type II supernovae (in which neutrinos push out baryons), the production of R Coronae Borealis stars (previously-owned baryons), and perhaps found the missing satellite galaxies (whose failing is that they have no baryons). A few questions were left unanswered for next year, and an attempt is made to discuss these as well.

show abstract

“…Before the establishment of the currently standard cosmology Ω m = 0.3 and Ω Λ = 0.7 (Riess et al 1998;Perlmutter et al 1999;Phillips et al 2001;Tonry et al 2003), various surveys have obtained measures of the galaxy two-point correlation function in redshift space and/or projected separation assuming either a low or high matter density Universe and a null cosmological constant (at z 0.1−0.5: Cole et al 1994;Le Fevre et al 1996;Small et al 1999;Guzzo et al 2000;Hogg et al 2000;Carlberg et al 2000;Shepherd et al 2001; at z 0: Loveday et al 1992;Park et al 1994;Baugh 1996;Tucker et al 1997;Ratcliffe et al 1998b;Giuricin et al 2001). To compare our results with those from the other surveys, we thus consider only the more recent measurements, which use the new standard cosmological parameters.…”

Section: Comparison With Other Surveysmentioning

confidence: 99%

“…Throughout the present analysis, we assume a flat Universe with, at the present epoch, a scale parameter H 0 = 100 h km s −1 Mpc −1 , a matter density Ω m = 0.3 and a cosmological energy density Ω Λ = 0.7 (Riess et al 1998;Perlmutter et al 1999;Phillips et al 2001;Tonry et al 2003). All absolute absolute magnitude are defined modulo +5 log h.…”

Section: Introductionmentioning

confidence: 99%

Spatial clustering in the ESO-Sculptor survey: two-point correlation functions by galaxy type at redshifts 0.1–0.5

Lapparent¹,

Slezak²

2007

A&A

View full text Add to dashboard Cite

Context. Galaxy clustering shows segregation effects with galaxy type, color and luminosity, which bring clues on the relationship with the underlying density field. Aims. We explore these effects among the populations of giant and dwarf galaxies detected in the ESO-Sculptor survey. Methods. We calculate the spatial two-point auto and cross-correlation functions for the 765 galaxies with R c ≤ 21.5 and 0.1 ≤ z ≤ 0.51 and for subsets by spectral type and luminosity. Results. At separation of 0.3 h −1 Mpc, pairs of early-type galaxies dominate the clustering over all the other types of pairs. At intermediate scales, 0.3−5 h −1 Mpc, mixed pairs of dwarf and giant galaxies contribute equally as pairs of giant galaxies, whereas the latter dominate at 10 h −1 Mpc. Moreover, the correlation functions per galaxy type display the expected transition between the 1-halo and 2-halo regimes in the scenario of hierarchical merging of dark matter halos. The 1-halo component of the early-type galaxies largely outdoes that for the late spiral galaxies, and that for the dwarf galaxies is intermediate between both. In contrast, the 2-halo component of the early-type galaxies and late spiral galaxies are comparable, whereas that for the dwarf galaxies is consistent with null clustering. Conclusions. We link the clustering segregation of the early-type and late spiral galaxies to their spatial distribution within the underlying dark matter halos. The early-type galaxies are preferentially located near the centers of the most massive halos, whereas late spiral galaxies tend to occupy their outskirts or the centers of less massive halos. This appears to be independent of luminosity for the early-type galaxies, whereas faint late spiral galaxies might reside in less dense regions than their bright analogs. The present analysis also unveils unprecedented results on the contribution from dwarf galaxies: at the scale at which they significantly cluster inside the halos (≤0.3 h −1 Mpc), they are poorly mixed with the late spiral galaxies, and appear preferentially as satellites of early-type galaxies.

show abstract

Constraints on Cosmological Parameters from the Lyα Forest Power Spectrum andCOBEDMR

Cited by 36 publications

References 61 publications

The ESO-Sculptor Survey: Evolution of late-type galaxies at redshifts 0.1–0.5

The ESO-Sculptor Survey: Evolution of late-type galaxies at redshifts 0.1–0.5

Astrophysics in 2002

Spatial clustering in the ESO-Sculptor survey: two-point correlation functions by galaxy type at redshifts 0.1–0.5

Contact Info

Product

Resources

About