INFALL OF NEARBY GALAXIES INTO THE VIRGO CLUSTER AS TRACED WITH<i>HUBBLE SPACE TELESCOPE</i>

Караченцев, И. Д.; Tully, R. Brent; Wu, Po-Feng; Shaya, E.; Dolphin, Andrew E.

doi:10.1088/0004-637x/782/1/4

Cited by 89 publications

(119 citation statements)

References 52 publications

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“…The centre of the LSC, the Virgo cluster at a distance of 16.5 Mpc ("Vir 1 ") has a virial mass ≈0.7 × 10 15 M within 1.8 Mpc. The zone of infall (up to 7 Mpc) may have one fifth of that mass (Karachentsev et al 2014). The mass further up towards the LG distance is not well known.…”

Section: Example Systems Of Galaxiesmentioning

confidence: 99%

A graph of dark energy significance on different spatial and mass scales

Teerikorpi

Heinämäki

Nurmi

et al. 2015

A&A

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Context. The current cosmological paradigm sees the formation and evolution of the cosmic large-scale structure as governed by the gravitational attraction of dark matter (DM) and the repulsion of dark energy (DE). Aims. We characterize the relative importance of uniform and constant dark energy, as given by the Λ term in the standard ΛCDM cosmology, in galaxy systems of different scales from groups to superclusters.Methods. An instructive "Λ significance graph" is introduced where the matter-DE density ratio ρ M /ρ Λ for different galaxy systems is plotted against the radius R. This presents gravitation-and DE-dominated regions and directly shows the zero velocity radius, the zero-gravity radius, and the Einstein-Straus radius for any fixed value of mass. Results. Example galaxy groups and clusters from the local universe illustrate the use of the Λ significance graph. These are generally located deep in the gravity-dominated region ρ M /ρ Λ > 2, and are virialized. Extended clusters and the main bodies of superclusters can reach down near the borderline between gravity-dominated and DE-dominated regions ρ M /ρ Λ = 2. The scale-mass relation from the standard two-point correlation function intersects this balance line near the correlation length. Conclusions. The log ρ M /ρ Λ vs. log R diagram is a useful and versatile way to characterize the dynamical state of systems of galaxies within the Λ-dominated expanding universe.

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Section: Example Systems Of Galaxiesmentioning

confidence: 99%

A graph of dark energy significance on different spatial and mass scales

Teerikorpi

Heinämäki

Nurmi

et al. 2015

A&A

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“…The galaxy groups 'NGC3998' and 'NGC3079' (in the North) are not considered to be bound to the Virgo cluster due to the large projected distance (Rp > 12 Mpc) and therefore unfeasible merging times. South of the filamentary structure resides the Virgo cluster (centred at α = 187.70, δ = 12.34 and v LG = 975 km s −1 ; Karachentsev et al 2014). The analysis of bound structures using the Newtonian binding criterion presented above can be used to determine if the Ursa Major region as a whole is bound to the nearby Virgo cluster.…”

Section: Will Ursa Major and Virgo Merge?mentioning

confidence: 99%

“…The analysis of bound structures using the Newtonian binding criterion presented above can be used to determine if the Ursa Major region as a whole is bound to the nearby Virgo cluster. The Virgo cluster has a total mass of M T = 8.0 × 10 14 M (Karachentsev et al 2014). Assuming that the still forming galaxy groups identified using strict linking lengths will eventually merge to form larger structures, the large-scale structures of the Ursa Major region as a whole may be bound to the Virgo cluster.…”

Section: Will Ursa Major and Virgo Merge?mentioning

confidence: 99%

“…The Ursa Major -Virgo region is shown in Figure 25 with the structures labelled in the top panel. For illustrative purposes a virial radius of R v = 1.8 Mpc (Karachentsev et al 2014) is assumed for the Virgo cluster. The twobody systems with probabilities P bound > 0 per cent are shown in Figure 25 (bottom; the probabilities are given as a numerical values in per cent).…”

Section: Will Ursa Major and Virgo Merge?mentioning

confidence: 99%

“…Using looser linking lengths (D 0 = 0.43 Mpc and V 0 = 120 km s −1 ) results in the NGC4026, NGC3938, NGC4449 and MESSIER106 groups being merged giving an estimate of the properties of the supergroup: a poor cluster with 185 galaxies, a velocity dispersion of 205 km s −1 , an early-type fraction of 23 per cent and a virial mass of 7.96 × 10 13 M . The zone of infall into the Virgo cluster has previously been determined to be 4 times the virial radius (highlighted in green; Karachentsev et al 2014).The Virgo cluster is likely to be accreting galaxy groups such as the NGC4274, NGC4725 and NGC3301 groups as well as the Ursa Major supergroup (marked with arrows towards the Virgo cluster). Note that the NGC4274 group was determined to be likely bound to the NGC3938 and NGC5033 groups (see Section 4.4).…”

Section: The Nature Of the Ursa Major Regionmentioning

confidence: 99%

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The Ursa Major Cluster Redefined as a ‘Supergroup’

Wolfinger

Kilborn

Ryan-Weber

et al. 2016

Publ. Astron. Soc. Aust.

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We identify gravitationally bound structures in the Ursa Major region using positions, velocities and photometry from the Sloan Digital Sky Survey (SDSS DR7) and the Third Reference Catalogue of Bright Galaxies (RC3). A friends-of-friends algorithm is extensively tested on mock galaxy lightcones and then implemented on the real data to determine galaxy groups whose members are likely to be physically and dynamically associated with one another. We find several galaxy groups within the region that are likely bound to one another and in the process of merging. We classify 6 galaxy groups as the Ursa Major 'supergroup', which are likely to merge and form a poor cluster with a mass of ∼ 8 × 10 13 M . Furthermore, the Ursa Major supergroup as a whole is likely bound to the Virgo cluster, which will eventually form an even larger system in the context of hierarchical structure formation.To investigate the evolutionary state of the galaxy groups in the Ursa Major region, we examine the location of the brightest group galaxy (BGG) as well as galaxy properties such as colour, morphological type, luminosity and HI content. The galaxy properties are examined with respect to group/non-group membership as well as a function of their local projected surface density. We find that (i) the BGGs often show a relatively large spatial and kinematic offset from the group centres, (ii) the increase in the fraction of early-type galaxies with local projected surface density is shallow, (iii) galaxy colours tend to be redder with increasing density, (iv ) there is no trend towards brighter galaxies with increasing density and (v ) several galaxies with HI excess are found in low density environments, whereas HI deficient galaxies tend to reside in the galaxy groups. We note that several galaxy groups contain members with disturbed HI content or HI tails. Given the low velocity dispersion of the groups and the lack of X-ray emission, these disturbances are likely due to galaxy-galaxy interactions. We conclude that the galaxy groups in the Ursa Major region are in an early evolutionary state and the properties of their member galaxies are similar to those in the field.

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Stellar and dark matter density in the Local Universe

Караченцев

Telikova

2018

Astron Nachr

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We calculate the mean density profiles for luminous and dark matter on distance scales D ∼ 1-100 Mpc around us using recent all-sky catalogs of galaxy groups. Within the Local Volume (D < 11 Mpc), we derived the mean stellar density Ω * = 0.44% in the critical density units and the mean total matter density Ω m = 0.17. Within a sphere of radius 40 Mpc, these quantities drop to Ω * = 0.24-0.32% and Ω m = 0.09-0.14. In a larger volume within D ∼ 135 Mpc, the discussed densities become more uncertain: Ω * = 0.20-0.24% and Ω m = 0.05-0.16. We summarize that the major part of the cosmic dark matter is located outside the virial and collapsing zones of groups and clusters.

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INFALL OF NEARBY GALAXIES INTO THE VIRGO CLUSTER AS TRACED WITHHUBBLE SPACE TELESCOPE

Cited by 89 publications

References 52 publications

A graph of dark energy significance on different spatial and mass scales

A graph of dark energy significance on different spatial and mass scales

The Ursa Major Cluster Redefined as a ‘Supergroup’

Stellar and dark matter density in the Local Universe

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