The cold local Hubble flow as a signature of dark energy

Baryshev, Yu. V.; Chernin, A. D.; Teerikorpi, P.

doi:10.1051/0004-6361:20011257

Cited by 69 publications

(92 citation statements)

References 42 publications

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“…Chernin 2001Ekholm et al 2001;Baryshev et al 2001;Byrd et al 2007;Niemi et al 2007;Teerikorpi et al 2008). Study of the Local Group enables one to learn not only the mass in the system, but simultaneusly, the local density of the dark energy itself.…”

Section: Discussionmentioning

confidence: 99%

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Local dark matter and dark energy as estimated on a scale of ~1 Mpc in a self-consistent way

Chernin¹,

Teerikorpi²,

Valtonen³

et al. 2009

A&A

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Context. Dark energy was first detected from large distances on gigaparsec scales. If it is vacuum energy (or Einstein's Λ), it should also exist in very local space. Here we discuss its measurement on megaparsec scales of the Local Group. Aims. We combine the modified Kahn-Woltjer method for the Milky Way-M 31 binary and the HST observations of the expansion flow around the Local Group in order to study in a self-consistent way and simultaneously the local density of dark energy and the dark matter mass contained within the Local Group. Methods. A theoretical model is used that accounts for the dynamical effects of dark energy on a scale of ∼1 Mpc. Results. The local dark energy density is put into the range 0.8−3.7ρ v (ρ v is the globally measured density), and the Local Group mass lies within 3.1−5.8 × 10 12 M . The lower limit of the local dark energy density, about 4/5× the global value, is determined by the natural binding condition for the group binary and the maximal zero-gravity radius. The near coincidence of two values measured with independent methods on scales differing by ∼1000 times is remarkable. The mass ∼4 × 10 12 M and the local dark energy density ∼ρ v are also consistent with the expansion flow close to the Local Group, within the standard cosmological model. Conclusions. One should take into account the dark energy in dynamical mass estimation methods for galaxy groups, including the virial theorem. Our analysis gives new strong evidence in favor of Einstein's idea of the universal antigravity described by the cosmological constant.

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Section: Discussionmentioning

confidence: 99%

“…Gravity and antigravity are exactly balanced at the zero-gravity surface of the radius R = R v (Chernin et al 2000;Chernin 2001;Baryshev et al 2001;Dolgachev et al 2003):…”

Section: Zero-gravity Radiusmentioning

confidence: 99%

Local dark matter and dark energy as estimated on a scale of ~1 Mpc in a self-consistent way

Chernin¹,

Teerikorpi²,

Valtonen³

et al. 2009

A&A

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“…It is important for our discussion that dark energy (initially discovered at horizon-scale distances) affects not only global cosmic dynamics, but also the dynamics on scales of galaxy groups, clusters and superclusters (Chernin et al 2000;Baryshev et al 2001;Nowakowski et al 2002;Karachentsev et al 2003;Manera & Mota 2006;Nunes & Mota 2006;Peirani & Freitas Pacheco 2006). Because the general properties of dark energy are universal, we may borrow their description from the cosmological model and General Relativity (e.g., the Kötler solution or Schwarzschild-de Sitter spacetime, Einstein-Straus model, etc.).…”

Section: Extended Dark Halos?mentioning

confidence: 99%

“…(10) gives its maximal radial size: R ZG = 1 Mpc. Because the observed radial size of the group is just near 1 Mpc (van den Bergh 1999;Karachentsev 2005;, one may conclude that the dark halo of the Local Group has the maximal possible size, R LG = R ZG , and therefore its observed mass is the maximal possible one: (Chernin et al 2000;Baryshev et al 2001;Chernin et al 2007a).…”

Section: Zero-gravity Radiusmentioning

confidence: 99%

Dark energy and extended dark matter halos

Chernin

Teerikorpi

Valtonen

et al. 2012

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The cosmological mean matter (dark and baryonic) density measured in the units of the critical density is Ω m = 0.27. Independently, the local mean density is estimated to be Ω loc = 0.08−0.23 from recent data on galaxy groups at redshifts up to z = 0.01−0.03 (as published by Crook et al. 2007, ApJ, 655, 790 and Makarov & Karachentsev 2011, MNRAS, 412, 2498. If the lower values of Ω loc are reliable, as Makarov & Karachentsev and some other observers prefer, does this mean that the Local Universe of 100-300 Mpc across is an underdensity in the cosmic matter distribution? Or could it nevertheless be representative of the mean cosmic density or even be an overdensity due to the Local Supercluster therein. We focus on dark matter halos of groups of galaxies and check how much dark mass the invisible outer layers of the halos are able to host. The outer layers are usually devoid of bright galaxies and cannot be seen at large distances. The key factor which bounds the size of an isolated halo is the local antigravity produced by the omnipresent background of dark energy. A gravitationally bound halo does not extend beyond the zero-gravity surface where the gravity of matter and the antigravity of dark energy balance, thus defining a natural upper size of a system. We use our theory of local dynamical effects of dark energy to estimate the maximal sizes and masses of the extended dark halos. Using data from three recent catalogs of galaxy groups, we show that the calculated mass bounds conform with the assumption that a significant amount of dark matter is located in the invisible outer parts of the extended halos, sufficient to fill the gap between the observed and expected local matter density. Nearby groups of galaxies and the Virgo cluster have dark halos which seem to extend up to their zero-gravity surfaces. If the extended halo is a common feature of gravitationally bound systems on scales of galaxy groups and clusters, the Local Universe could be typical or even an overdense region, with a low density contrast ∼1.

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“…As a new and numerous target group in extragalactic studies dEs serve also to test the peculiar linearity and smoothness of the Hubble flow in the local volume. As such they may help to define, or at least refine, the dark energy solution to the problem (Baryshev et al 2001).…”

Section: Introductionmentioning

confidence: 99%

New distances of unresolved dwarf elliptical galaxies in the vicinity of the Local Group

Rekola

Jerjen

Flynn

2005

A&A

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Abstract. We present Surface Brightness Fluctuation distances of nine early-type dwarf galaxies and the S0 galaxy NGC 4150 in the Local Volume based on deep B-and R-band CCD images obtained with the 2.56 m Nordic Optical Telescope. Typically, six stellar fields at various galactocentric distances have been chosen for each galaxy as appropriately free of foreground stars and other contaminants, and Fourier analysed to determine the distances, which are found to lie in the range of 3 to 16 Mpc. The SBF method is thus demonstrated to efficiently measure distances from the ground with mid-aperture telescopes for galaxies for which only the tip of the red giant branch method in combination with the Hubble Space Telescope has been available until now. We obtained the following distance moduli: 28.11 ± 0.15 mag (or 4.2 ± 0.3 Mpc) for UGC 1703, 27.61 ± 0.17 mag (or 3.3 ± 0.3 Mpc) for KDG 61, 29.00 ± 0.27 mag (or 6.3 ± 0.8 Mpc) for UGCA 200, 27.74 ± 0.18 mag (or 3.5 ± 0.3 Mpc) for UGC 5442, 30.22 ± 0.17 mag (or 11.1 ± 0.9 Mpc) for UGC 5944, 30.79 ± 0.11 mag (or 14.4 ± 0.7 Mpc) for NGC 4150, 31.02 ± 0.25 mag (or 16.0 ± 1.9 Mpc) for BTS 128, 29.27 ± 0.16 mag (or 7.1 ± 0.6 Mpc) for UGC 7639, 30.19 ± 0.23 mag (or 10.9 ± 1.2 Mpc) for UGC 8799 with an alternative distance of 30.61 ± 0.26 mag (or 13.2 ± 1.7 Mpc), and 29.60 ± 0.20 mag (or 8.3 ± 0.8 Mpc) for UGC 8882.

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The cold local Hubble flow as a signature of dark energy

Cited by 69 publications

References 42 publications

Local dark matter and dark energy as estimated on a scale of ~1 Mpc in a self-consistent way

Local dark matter and dark energy as estimated on a scale of ~1 Mpc in a self-consistent way

Dark energy and extended dark matter halos

New distances of unresolved dwarf elliptical galaxies in the vicinity of the Local Group

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