Gravitational lensing statistics with extragalactic surveys

Helbig, Phillip; Marlow, D. R.; Quast, Ralf; Wilkinson, P. N.; Browne, I. W. A.; Koopmans, L. V. E.

doi:10.1051/aas:1999467

Cited by 48 publications

(79 citation statements)

References 13 publications

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“…Present estimates (Falco, Kochanek, and Muñoz, 1998;Helbig et al, 1999) do not seriously constrain Ω M0 in an open model, and in a flat model (Ω K0 = 0) suggest Ω M0 > 0.36 at 2σ. This is close to the upper bound in Eq.…”

Section: The Gravitational Lensing Ratementioning

confidence: 63%

The cosmological constant and dark energy

2003

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Physics invites the idea that space contains energy whose gravitational effect approximates that of Einstein's cosmological constant, Λ; nowadays the concept is termed dark energy or quintessence. Physics also suggests the dark energy could be dynamical, allowing the arguably appealing picture that the dark energy density is evolving to its natural value, zero, and is small now because the expanding universe is old. This alleviates the classical problem of the curious energy scale of order a millielectronvolt associated with a constant Λ. Dark energy may have been detected by recent advances in the cosmological tests. The tests establish a good scientific case for the context, in the relativistic Friedmann-Lemaître model, including the gravitational inverse square law applied to the scales of cosmology. We have well-checked evidence that the mean mass density is not much more than one quarter of the critical Einstein-de Sitter value. The case for detection of dark energy is serious but not yet as convincing; we await more checks that may come out of work in progress. Planned observations might be capable of detecting evolution of the dark energy density; a positive result would be a considerable stimulus to attempts to understand the microphysics of dark energy. This review presents the basic physics and astronomy of the subject, reviews the history of ideas, assesses the state of the observational evidence, and comments on recent developments in the search for a fundamental theory.

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Section: The Gravitational Lensing Ratementioning

confidence: 63%

The cosmological constant and dark energy

2003

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“…We note that recent studies of high-redshift Type Ia supernovae, the cosmic microwave background, and the statistics of gravitational lenses suggest that the universe is Ñat with a nonzero cosmological constant, " (see, e.g., Kochanek 1996 ;Helbig et al 1999 ;de Bernadis et al 2000 ;Pryke et al 2001 ;Riess et al 2001 and references therein). Currently, the preferred world model is and ) M B 0.35 In this cosmology, the log R values are almost ) " B 0.65. identical to the empty-universe case ; they are larger (q 0 \ 0) by only 0.01 dex or less at the redshifts of our three clusters.…”

Section: Sensitivity Of the Conclusion To The Assumptions That Andmentioning

confidence: 82%

The Tolman Surface Brightness Test for the Reality of the Expansion. IV. A Measurement of the Tolman Signal and the Luminosity Evolution of Early-Type Galaxies

Lubin

Sandage

2001

The Astronomical Journal

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We review a sample of the early literature in which the reality of the expansion is discussed. HubbleÏs reluctance, even as late as 1953, to accept the expansion as real is explained as due to his use of equations for distances and absolute magnitudes of redshifted galaxies that do not conform to the modern Mattig equations of the standard model. The Tolman surface brightness test, once the only known test for the reality of the expansion, is contrasted with three other modern tests. These are (1) the time dilation in Type Ia supernovae light curves, (2) the temperature of the relic radiation as a function of redshift, and (3) the surface brightness normalization of the Planckian shape of the relic radiation. We search for the Tolman surface brightness depression with redshift using the Hubble Space T elescope (HST ) data from Paper III for 34 early-type galaxies from the three clusters Cl 1324]3011 (z \ 0.76), Cl 1604]4304 (z \ 0.90), and Cl 1604]4321 (z \ 0.92). Depressions of the surface brightness relative to the zero-redshift Ðducial lines in the mean surface brightnessÈlogarithm of the linear radius diagrams of Paper I are found for all three clusters. Expressed as the exponent, n, in 2.5 log (1 ] z)n mag, the value of n averaged over Petrosian radii of g \ 1.7 and g \ 2.0 for all three clusters is n \ 2.59^0.17 in the R band and 3.37^0.13 in the I band for a model. The sensitivity of the result to the assumed q 0 \ 1/2 value of is shown to be less than 23% between q \ 0 and ]1. The conclusion is that the exponent on q 0 (1 ] z) varies from 2.28 to 2.81 (^0.17) in the R band and 3.06 to 3.55 (^0.13) in the I band, depending on the value of For a true Tolman signal with n \ 4, the luminosity evolution in the look-back time, q 0 . expressed as the exponent in 2.5 log (1 ] z)4~n mag, must then be between 1.72 to 1.19 (^0.17) in the R band and 0.94 to 0.45 (^0.13) in the I band. We show that this is precisely the range expected from the evolutionary models of Bruzual and Charlot and other measurements of the luminosity evolution of early-type galaxies. We conclude that the Tolman surface brightness test is consistent with the reality of the expansion to within the combined errors of the observed SSBT depression and the theoretical correction for luminosity evolution. We have also used the high-redshift HST data to test the "" tired light ÏÏ speculation for a nonexpansion model for the redshift. The HST data rule out the tired light model at a signiÐcance level of better than 10 p.

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“…A similar measurement using clusters of galaxies gives (90% con-) 0 0.6 p 8 \ 0.44~0 .13 0.19 Ðdence ; Watkins 1997, Borgani et al 1997. We compare the da Costa et al (1998) Corray, Quasnock, & Miller (1999 ;[0.21), Helbig et al (1999 ;[0.36), Chiba & Yoshii (1999 ; at 68% 0.3~0 .1 0.2 conÐdence), and Cheng & Krauss (1999 ;0.25È0.55 systematic e †ects dominate). All these results agree with what we Ðnd.…”

Section: Comparison With Other Measurementsmentioning

confidence: 91%

Measuring Cosmological Parameters from the Evolution of Cluster X‐Ray Temperatures

Henry¹

2000

ApJ

259

341

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We have determined the cluster X-ray temperature function from two Ñux-and redshift-limited samples of clusters. The Ðrst sample is comprised of 25 clusters with average redshift 0.05. The local temperature function derived from it supersedes the one we published previously. Fourteen clusters with average redshift 0.38 comprise the second sample. We perform maximum likelihood Ðts of cluster evolution models to these data in order to constrain cosmological parameters. For an open model with zero cosmological constant we Ðnd that the density parameter is the rms mass density Ñuc-) 0 \ 0.49^0.12, tuation averaged over 8 h~1 Mpc spheres is and the e †ective index of the mass density p 8 \ 0.72^0.10, Ñuctuation spectrum on cluster scales is n \ [(1.72^0.34), where all errors are symmetrized at 68% conÐdence. The corresponding results for the case where a cosmological constant produces a Ñat universe are 0. 44^0.12, 0.77^0.15, and [ (1.68^0.38). These results agree with those determined from a variety of di †erent independent methods, including supernovae, galaxy-galaxy correlations, Ñuctuations in the microwave background, gravitational lens statistics, and cluster peculiar velocities.

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Gravitational lensing statistics with extragalactic surveys

Cited by 48 publications

References 13 publications

The cosmological constant and dark energy

The cosmological constant and dark energy

The Tolman Surface Brightness Test for the Reality of the Expansion. IV. A Measurement of the Tolman Signal and the Luminosity Evolution of Early-Type Galaxies

Measuring Cosmological Parameters from the Evolution of Cluster X‐Ray Temperatures

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