DOI: 10.1126/science.287.5450.109. Evidence for a Low-Density Universe from the Relative Velocities of Galaxies

Evidence for a Low-Density Universe from the Relative Velocities of Galaxies

10.1126/science.287.5450.109

Crossref journal-article

American Association for the Advancement of Science (AAAS)

Science (221)

Abstract

The motions of galaxies can be used to constrain the cosmological density parameter Ω and the clustering amplitude of matter on large scales. The mean relative velocity of galaxy pairs, estimated from the Mark III survey, indicates that Ω = 0.35 −0.25 +0.35 . If the clustering of galaxies is unbiased on large scales, Ω = 0.35 ± 0.15, so that an unbiased Einstein–de Sitter model (Ω = 1) is inconsistent with the data.

Bibliography

Juszkiewicz, R., Ferreira, P. G., Feldman, H. A., Jaffe, A. H., & Davis, M. (2000). Evidence for a Low-Density Universe from the Relative Velocities of Galaxies. Science, 287(5450), 109â112.

Authors 5

R. Juszkiewicz (first)
P. G. Ferreira (additional)
H. A. Feldman (additional)
A. H. Jaffe (additional)
M. Davis (additional)

References 35 Referenced 54

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. To linear bias enthusiasts this result may appear puzzling. A textbook example of such a possibility is the spatial distribution of the gas and stars in a galaxy. Their distribution itself is biased whereas their relative velocities at separations comparable to the radius of the dark halo are not.
Strauss M. A., Willick J. A., Phys. Rep. 261, 271 (1995). (10.1016/0370-1573(95)00013-7) / Phys. Rep. by Strauss M. A. (1995)
N -body simulations show that the stable clustering solution [u 12 = 0 −v 12 (r)/Hr = 1] occurs for ξ > 200 [(7); see also
Jain B., Mon. Not. R. Astron. Soc. 287, 687 (1997); (10.1093/mnras/287.3.687) / Mon. Not. R. Astron. Soc. by Jain B. (1997)
]. In the limit r → 0 our ansatz gives −v 12 /Hr → [2/(3 − γ)]Ω 0.6 (1 + α) which for the range of parameters considered is generally different from unity (although of the right order of magnitude). It is possible to improve our approximation and satisfy the small separation boundary condition by replacing (2/3)Ω 0.6 with the expression [(1 − γ/3)Fξ(r) + (2/3)Ω 0.6 ]/[Fξ(r) + 1] where F ≈ 1/100 is a fudge factor ensuring that −v 12 /Hr → 1 when ξ » 100 while the perturbative large-scale solution remains unaffected. However the stable clustering occurs at separations smaller than 200h −1 kpc which is a tenth of the smallest separation we consider here. As a result in our range of separations r Eq. 1 is as close to fully nonlinear N -body simulations as the improvement suggested above [see (4) and Fig. 2].
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Under realistic circumstances one expects that gravitational growth of clustering pulls the mass with the galaxies. As a result any clustering bias introduced at the epoch of galaxy formation is likely to evolve toward unity at late times at variance with the linear bias model where b is time independent [
Fry J. N., Astrophys. J. 461, L65 (1996); / Astrophys. J. by Fry J. N. (1996)
; P. J. E. Peebles available at ]. A similar behavior was seen in N -body simulations (11). The linear bias relation δ gal = b δ is a conjecture that generally does not follow from the relation between the correlation functions ξ gal = b 2 ξ unless we restrict our model to a narrow subclass of random fields.
Imagine that one of the CDM-like models is a valid description of our universe. Let us choose the dark energy and CDM (ΛCDM) model recently simulated by the Virgo Consortium (7). It is defined by parameters h = 0.7 Ω = 0.3 σ 8 = 0.9 and Ω Λ = 0.7 which is the cosmological constant's contribution to the density parameter. This model requires scale-dependent biasing because the predicted shape of ξ(r) differs widely from the observed galaxy correlation function: At separations hr Mpc −1 = 10 4 2 and 0.1 the logarithmic slope of the mass correlation function reaches the values given by γ = 1.7 1.5 2.5 and 1 respectively. As we expected however these wild oscillations do not affect the resulting v 12 (r * ). Indeed the N -body simulations (7) give v 12 (r * ) = −220 km s −1 and substituting σ 8 = 0.9 and Ω = 0.3 in Eq. 5 gives v 12 (r * ) = −225 km s −1 .
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We are grateful to L. da Costa for encouragement at the early stages of this project. We also benefited from discussions with S. Courteau R. Durrer K. Górski and J. Peebles. R.J. was supported by the State Committee for Scientific Research (KBN) (Poland) the Tomalla Foundation (Switzerland) and the Poland-U.S. M. Skłodowska-Curie Fund. M.D. and A.H.J. were supported by grants from NSF and NASA. H.A.F. and R.J. were supported by NSF-EPSCOR and the General Research Fund. We thank the organizers of the summer 1997 workshop at the Aspen Center for Physics where this work began.

Dates

Type	When
Created	23 years ago (July 27, 2002, 5:35 a.m.)
Deposited	1 year, 7 months ago (Jan. 13, 2024, 4:51 a.m.)
Indexed	1 month, 3 weeks ago (July 2, 2025, 3:27 p.m.)
Issued	25 years, 7 months ago (Jan. 7, 2000)
Published	25 years, 7 months ago (Jan. 7, 2000)
Published Print	25 years, 7 months ago (Jan. 7, 2000)

Funders 0

None

BibTeX

@article{Juszkiewicz_2000, title={Evidence for a Low-Density Universe from the Relative Velocities of Galaxies}, volume={287}, ISSN={1095-9203}, url={http://dx.doi.org/10.1126/science.287.5450.109}, DOI={10.1126/science.287.5450.109}, number={5450}, journal={Science}, publisher={American Association for the Advancement of Science (AAAS)}, author={Juszkiewicz, R. and Ferreira, P. G. and Feldman, H. A. and Jaffe, A. H. and Davis, M.}, year={2000}, month=jan, pages={109–112} }

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  "abstract": "<jats:p>\n            The motions of galaxies can be used to constrain the cosmological density parameter \u03a9 and the clustering amplitude of matter on large scales. The mean relative velocity of galaxy pairs, estimated from the Mark III survey, indicates that \u03a9 = 0.35\n            <jats:sub>\u22120.25</jats:sub>\n            <jats:sup>+0.35</jats:sup>\n            . If the clustering of galaxies is unbiased on large scales, \u03a9 = 0.35 \u00b1 0.15, so that an unbiased Einstein\u2013de Sitter model (\u03a9 = 1) is inconsistent with the data.\n          </jats:p>",
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      "unstructured": "]. In the limit r \u2192 0 our ansatz gives \u2212v 12 /Hr \u2192 [2/(3 \u2212 \u03b3)]\u03a9 0.6 (1 + \u03b1) which for the range of parameters considered is generally different from unity (although of the right order of magnitude). It is possible to improve our approximation and satisfy the small separation boundary condition by replacing (2/3)\u03a9 0.6 with the expression [(1 \u2212 \u03b3/3)F\u03be(r) + (2/3)\u03a9 0.6 ]/[F\u03be(r) + 1] where F \u2248 1/100 is a fudge factor ensuring that \u2212v 12 /Hr \u2192 1 when \u03be \u00bb 100 while the perturbative large-scale solution remains unaffected. However the stable clustering occurs at separations smaller than 200h \u22121 kpc which is a tenth of the smallest separation we consider here. As a result in our range of separations r Eq. 1 is as close to fully nonlinear N -body simulations as the improvement suggested above [see (4) and Fig. 2]."
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      "unstructured": "; P. J. E. Peebles available at ]. A similar behavior was seen in N -body simulations (11). The linear bias relation \u03b4 gal = b \u03b4 is a conjecture that generally does not follow from the relation between the correlation functions \u03be gal = b 2 \u03be unless we restrict our model to a narrow subclass of random fields."
    },
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      "unstructured": "Imagine that one of the CDM-like models is a valid description of our universe. Let us choose the dark energy and CDM (\u039bCDM) model recently simulated by the Virgo Consortium (7). It is defined by parameters h = 0.7 \u03a9 = 0.3 \u03c3 8 = 0.9 and \u03a9 \u039b = 0.7 which is the cosmological constant's contribution to the density parameter. This model requires scale-dependent biasing because the predicted shape of \u03be(r) differs widely from the observed galaxy correlation function: At separations hr Mpc \u22121 = 10 4 2 and 0.1 the logarithmic slope of the mass correlation function reaches the values given by \u03b3 = 1.7 1.5 2.5 and 1 respectively. As we expected however these wild oscillations do not affect the resulting v 12 (r * ). Indeed the N -body simulations (7) give v 12 (r * ) = \u2212220 km s \u22121 and substituting \u03c3 8 = 0.9 and \u03a9 = 0.3 in Eq. 5 gives v 12 (r * ) = \u2212225 km s \u22121 ."
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