Limits on cold dark matter cosmologies from new anisotropy bounds on the cosmic microwave background

Vittorio, N.; Meinhold, P. R.; Lubin, P. M.; Muciaccia, Pio Francesco; Silk, Joseph

doi:10.1086/186009

Cited by 26 publications

(10 citation statements)

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“…The Cosmic Background Explorer (COBE) has detected anisotropy at large angular scales (>5°) (Smoot et al 1992). Anisotropy measurements on medium angular scales constrain models of large-scale structure formation and the values of certain global parameters in cosmic evolution models (Bond et al 1991;Vittorio et al 1991). More powerful tests of cosmological models are possible when these measurements are combined with the measurements from COBE.…”

Section: Introductionmentioning

confidence: 99%

Measurements of anisotropy in the cosmic microwave background radiation at 0.5 deg angular scales near the star gamma ursae minoris

Devlin

Clapp

Gundersen

et al. 1994

ApJ

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We present results from a four frequency observation of a 6° x 0°.6 strip of the sky centered near the star Gamma Ursae Minoris during the fourth flight of the Millimeter-wave Anisotropy eXperiment (MAX). The observation was made with a 1°.4 peak-to-peak sinusoidal chop in all bands. The FWHM beam sizes were 0°.55 ± 0°.05 at 3.5 cm -1 and 0°.75 ± 0°.05 at 6, 9, and 14 cm -1 . During this observation significant correlated structure was observed at 3.5, 6 and 9 cm -1 with amplitudes similar to those observed in the GUM region during the second and third flights of MAX. The frequency spectrum is consistent with CMB and inconsistent with thermal emission from interstellar dust. The extrapolated amplitudes of synchrotron and free-free emission are too small to account for the amplitude of the observed structure. If all of the structure is attributed to CMB anisotropy with a Gaussian autocorrelation function and a coherence angle of 25', then the most probable values of ∆T/T CMB in the 3.5, 6, and 9 cm -1 bands are 4.3 −1.6 +2.7 × 10 −5 , 2.8 −1.1 +4.3 × 10 −5 , and 3.5 −1.6 +3.0 × 10 −5 (95% confidence upper and lower limits), respectively.

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Section: Introductionmentioning

confidence: 99%

Measurements of anisotropy in the cosmic microwave background radiation at 0.5 deg angular scales near the star gamma ursae minoris

Devlin

Clapp

Gundersen

et al. 1994

ApJ

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“…Tully 1988; Leonard and Lake 1995). Alternatively, if we assume Ω 0 = 1, Ω Λ = 0 and inflation we run into problems with the results of the anisotropy measurements of the cosmic microwave background (Bond et al 1991;Vittorio et al 1991). Furthermore, recent calculations based on cosmic nucleosynthesis together with the presently available observational estimates on the abundances of light elements (see Gerhard and Silk 1996 and references therein) have put limits on Ω M within the range 0 · 01 < Ω M h 2 < 0·02 (h is the Hubble constant in units of 100 km/s/Mpc).…”

Section: Discussionmentioning

confidence: 99%

Implications of a Nonzero Cosmological Constant and Luminosity Selection Effects on Cosmological Tests

Ubachukwu¹

1998

Aust. J. Phys.

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This paper examines the implications of a nonzero cosmological constant Λ0 on the amount of linear size evolution and the luminosity selection effects usually required in the interpretation of the angular diameter-redshift (θ-z) test. This is based on three typical cases chosen on various plausible assumptions which can be made concerning the contribution of Λ0 to the density of the universe (parametrised by Ω0). The results show that a fairly strong linear size evolution will be required to interpret the θ-z data of extended steep spectrum quasars for all three cases, if luminosity effects are neglected. However, this evolution is significantly steeper in a matter-dominated universe with Ω M = Ω0 = 1 than in both the flat universe with Ω Λ = 0·8, Ω M = 0·2 and an open universe with Ω M = 0·2, Ω Λ = 0.Furthermore, when the luminosity selection effects present in the sample are considered, a milder size evolution is obtained for the Ω M = 1, Ω Λ = 0 model while little or no size evolution is found for the other two cases. There is therefore no significant difference in our results for an open low density universe with Ω Λ = 0 and a flat universe dominated by Ω Λ predicted by inflation. The present results therefore imply that an open low density universe with Ω M = 0·2 and Ω Λ = 0 is compatible with an inflationary model of the universe with Ω M = 0·2 and Ω Λ = 0·8. This leads to a contradiction since the universe cannot be open and spatially closed at the same time (the existence of one should preclude the other).

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“…If the top-down model is correct, then the large earliest structures would have a distorting effect on the Cosmic Microwave Background (CMB) radiation, which is not seen to the current lowest determinations of A T /T on even the smallest angular scales (Bond and Efstathiou, 1984, Vittorio and Silk, 1984, Vittorio, Meinhold, Muciaccia, Lubin and Silk, 1991. This would appear to rule out the "top-down" scenario entirely.…”

Section: O N C O Sm O Lo G Ic a L T Im E An D D Is Ta N C E S Ca Lesmentioning

confidence: 97%

Dark Matter in Spiral Galaxies

Buchhorn

1993

Publ. Astron. Soc. Aust.

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Limits on cold dark matter cosmologies from new anisotropy bounds on the cosmic microwave background

Cited by 26 publications

References 0 publications

Measurements of anisotropy in the cosmic microwave background radiation at 0.5 deg angular scales near the star gamma ursae minoris

Measurements of anisotropy in the cosmic microwave background radiation at 0.5 deg angular scales near the star gamma ursae minoris

Implications of a Nonzero Cosmological Constant and Luminosity Selection Effects on Cosmological Tests

Dark Matter in Spiral Galaxies

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