Constraints on (Ωm, ΩΛ) using distributions of inclination angles for high redshift filaments

Research output: Contribution to journal › Journal article › Research › peer-review

Standard

Constraints on (Ωm, ΩΛ) using distributions of inclination angles for high redshift filaments. / Weidinger, M.; Møller, P.; Fynbo, J. P.U.; Thomsen, B.; Egholm, M. P.

In: Astronomy and Astrophysics, Vol. 391, No. 1, 08.2002, p. 13-20.

Research output: Contribution to journal › Journal article › Research › peer-review

Harvard

Weidinger, M, Møller, P, Fynbo, JPU, Thomsen, B & Egholm, MP 2002, 'Constraints on (Ωm, ΩΛ) using distributions of inclination angles for high redshift filaments', Astronomy and Astrophysics, vol. 391, no. 1, pp. 13-20. https://doi.org/10.1051/0004-6361:20020792

APA

Weidinger, M., Møller, P., Fynbo, J. P. U., Thomsen, B., & Egholm, M. P. (2002). Constraints on (Ωm, ΩΛ) using distributions of inclination angles for high redshift filaments. Astronomy and Astrophysics, 391(1), 13-20. https://doi.org/10.1051/0004-6361:20020792

Vancouver

Weidinger M, Møller P, Fynbo JPU, Thomsen B, Egholm MP. Constraints on (Ωm, ΩΛ) using distributions of inclination angles for high redshift filaments. Astronomy and Astrophysics. 2002 Aug;391(1):13-20. https://doi.org/10.1051/0004-6361:20020792

Author

Weidinger, M. ; Møller, P. ; Fynbo, J. P.U. ; Thomsen, B. ; Egholm, M. P. / Constraints on (Ωm, ΩΛ) using distributions of inclination angles for high redshift filaments. In: Astronomy and Astrophysics. 2002 ; Vol. 391, No. 1. pp. 13-20.

Bibtex

@article{8ba46c2fa4524193baa9653dc6ee13f5,
title = "Constraints on (Ωm, ΩΛ) using distributions of inclination angles for high redshift filaments",
abstract = "In this paper we present a scale free method to determine the cosmological parameters (Ωm, ΩΔ). The method is based on the requirement of isotropy of the distribution of orientations of cosmological filaments. The current structure formation paradigm predicts that the first structures to form are voids and filaments, causing a web-like structure of the matter distribution at high redshifts. Recent observational evidence suggests that the threads, or filaments, of the cosmic web most easily are mapped in Lyα emission. We describe how such a 3D map can be used to constrain the cosmological parameters in a way which, contrary to most other cosmological tests, does not require the use of a standard rod or a standard candle. We perform detailed simulations in order to define the optimal survey parameters for the definition of an observing programme aimed to address this test, and to investigate how statistical and observational errors will influence the results. We conclude that observations should target filaments of comoving size 15-50 Mpc in the redshift range 2-4, and that each filament must be defined by at least four Lyα emitters. Detection of 20 filaments will be sufficient to obtain a result, while 50 filaments will make it possible to place significant new constraints on the values of Ωm and ΩΛ permitted by the current supernova observations. In a future paper we study how robust these conclusions are to systematic velocities in the survey box.",
keywords = "Cosmological parameters, Cosmology: theory",
author = "M. Weidinger and P. M{\o}ller and Fynbo, {J. P.U.} and B. Thomsen and Egholm, {M. P.}",
year = "2002",
month = aug,
doi = "10.1051/0004-6361:20020792",
language = "English",
volume = "391",
pages = "13--20",
journal = "Astronomy & Astrophysics",
issn = "0004-6361",
publisher = "E D P Sciences",
number = "1",

}

RIS

TY - JOUR

T1 - Constraints on (Ωm, ΩΛ) using distributions of inclination angles for high redshift filaments

AU - Weidinger, M.

AU - Møller, P.

AU - Fynbo, J. P.U.

AU - Thomsen, B.

AU - Egholm, M. P.

PY - 2002/8

Y1 - 2002/8

N2 - In this paper we present a scale free method to determine the cosmological parameters (Ωm, ΩΔ). The method is based on the requirement of isotropy of the distribution of orientations of cosmological filaments. The current structure formation paradigm predicts that the first structures to form are voids and filaments, causing a web-like structure of the matter distribution at high redshifts. Recent observational evidence suggests that the threads, or filaments, of the cosmic web most easily are mapped in Lyα emission. We describe how such a 3D map can be used to constrain the cosmological parameters in a way which, contrary to most other cosmological tests, does not require the use of a standard rod or a standard candle. We perform detailed simulations in order to define the optimal survey parameters for the definition of an observing programme aimed to address this test, and to investigate how statistical and observational errors will influence the results. We conclude that observations should target filaments of comoving size 15-50 Mpc in the redshift range 2-4, and that each filament must be defined by at least four Lyα emitters. Detection of 20 filaments will be sufficient to obtain a result, while 50 filaments will make it possible to place significant new constraints on the values of Ωm and ΩΛ permitted by the current supernova observations. In a future paper we study how robust these conclusions are to systematic velocities in the survey box.

AB - In this paper we present a scale free method to determine the cosmological parameters (Ωm, ΩΔ). The method is based on the requirement of isotropy of the distribution of orientations of cosmological filaments. The current structure formation paradigm predicts that the first structures to form are voids and filaments, causing a web-like structure of the matter distribution at high redshifts. Recent observational evidence suggests that the threads, or filaments, of the cosmic web most easily are mapped in Lyα emission. We describe how such a 3D map can be used to constrain the cosmological parameters in a way which, contrary to most other cosmological tests, does not require the use of a standard rod or a standard candle. We perform detailed simulations in order to define the optimal survey parameters for the definition of an observing programme aimed to address this test, and to investigate how statistical and observational errors will influence the results. We conclude that observations should target filaments of comoving size 15-50 Mpc in the redshift range 2-4, and that each filament must be defined by at least four Lyα emitters. Detection of 20 filaments will be sufficient to obtain a result, while 50 filaments will make it possible to place significant new constraints on the values of Ωm and ΩΛ permitted by the current supernova observations. In a future paper we study how robust these conclusions are to systematic velocities in the survey box.

KW - Cosmological parameters

KW - Cosmology: theory

UR - http://www.scopus.com/inward/record.url?scp=0036685328&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:20020792

DO - 10.1051/0004-6361:20020792

M3 - Journal article

AN - SCOPUS:0036685328

VL - 391

SP - 13

EP - 20

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

IS - 1

ER -

ID: 243912389