Structure and kinematics of the Virgo cluster of galaxies

Kashibadze, O. G.; Караченцев, И. Д.; Караченцева, В. Е.

doi:10.1051/0004-6361/201936172

Cited by 49 publications

(41 citation statements)

References 39 publications

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“…Likely, the most massive halo in the LV is the Leo I group (for which we take NGC 3379 as the 'host') at M halo ∼ 10 13 M (Kourkchi & Tully 2017). On the other hand, the Fornax cluster has a dynamical mass of M 200 ∼ 7 × 10 13 M (Kourkchi & Tully 2017), noticeably less massive than the Virgo cluster which has an estimated mass closer to 5−6×10 14 M (Ferrarese et al 2012;Kourkchi & Tully 2017;Kashibadze et al 2020). Thus, the LV satellites are in halos generally at least an order of magnitude less massive than the environment of the cluster satellites.…”

Section: Effect Of Environmentmentioning

confidence: 99%

Structures of Dwarf Satellites of Milky Way-like Galaxies: Morphology, Scaling Relations, and Intrinsic Shapes

Carlsten

Greene

Greco

et al. 2021

ApJ

101

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The structure of a dwarf galaxy is an important probe of the effects of stellar feedback and environment. Using an unprecedented sample of 223 low-mass satellites from the ongoing Exploration of Local Volume Satellites survey, we explore the structures of dwarf satellites in the mass range 105.5 < M ⋆ < 108.5 M ⊙. We survey satellites around 80% of the massive, M K < − 22.4 mag, hosts in the Local Volume (LV). Our sample of dwarf satellites is complete to luminosities of M V <−9 mag and surface brightness μ 0,V < 26.5 mag arcsec−2 within at least ∼200 projected kpc of the hosts. For this sample, we find a median satellite luminosity of M V = −12.4 mag, median size of r e = 560 pc, median ellipticity of ϵ = 0.30, and median Sérsic index of n = 0.72. We separate the satellites into late- and early-type (29.6% and 70.4%, respectively). The mass–size relations are very similar between them within ∼5%, which indicates that the quenching and transformation of a late-type dwarf into an early-type one involves only very mild size evolution. Considering the distribution of apparent ellipticities, we infer the intrinsic shapes of the early- and late-type samples. Combining with literature samples, we find that both types of dwarfs are described roughly as oblate spheroids that get more spherical at fainter luminosities, but early-types are always rounder at fixed luminosity. Finally, we compare the LV satellites with dwarf samples from the cores of the Virgo and Fornax clusters. We find that the cluster satellites show similar scaling relations to the LV early-type dwarfs but are roughly 10% larger at fixed mass, which we interpret as being due to tidal heating in the cluster environments. The dwarf structure results presented here are a useful reference for simulations of dwarf galaxy formation and the transformation of dwarf irregulars into spheroidals.

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Section: Effect Of Environmentmentioning

confidence: 99%

Structures of Dwarf Satellites of Milky Way-like Galaxies: Morphology, Scaling Relations, and Intrinsic Shapes

Carlsten

Greene

Greco

et al. 2021

ApJ

101

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“…We can, like Bachchan et al (2016), estimate the acceleration due to nearby galaxy clusters from their estimated masses and distances. The Virgo cluster at a distance 16.5 Mpc (Mei et al 2007) and a mass (1.4−6.3) × 10 14 M (Ferrarese et al 2012;Kashibadze et al 2020) is the most significant single influence (0.002 to 0.010 km s −1 Myr −1 ). However, we recognise that the peculiar velocity of the Sun with respect to the Hubble flow has a component away from the Local Void, one towards the centre of the Laniakea supercluster, and others on larger scales that are not yet mapped (Tully et al 2008(Tully et al , 2014, and that this is probably reflected in the acceleration felt on the solar system barycentre from large scale structure.…”

Section: Specific Objectsmentioning

confidence: 99%

GaiaEarly Data Release 3

Klioner

Mignard

Lindegren

et al. 2021

A&A

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Context. Gaia Early Data Release 3 (Gaia EDR3) provides accurate astrometry for about 1.6 million compact (QSO-like) extragalactic sources, 1.2 million of which have the best-quality five-parameter astrometric solutions. Aims. The proper motions of QSO-like sources are used to reveal a systematic pattern due to the acceleration of the solar systembarycentre with respect to the rest frame of the Universe. Apart from being an important scientific result by itself, the acceleration measured in this way is a good quality indicator of the Gaia astrometric solution. Methods. Theeffect of the acceleration was obtained as a part of the general expansion of the vector field of proper motions in vector spherical harmonics (VSH). Various versions of the VSH fit and various subsets of the sources were tried and compared to get the most consistent result and a realistic estimate of its uncertainty. Additional tests with the Gaia astrometric solution were used to get a better idea of the possible systematic errors in the estimate. Results. Our best estimate of the acceleration based on Gaia EDR3 is (2.32 ± 0.16) × 10−10 m s−2 (or 7.33 ±0.51 km s−1 Myr−1) towards α = 269.1° ± 5.4°, δ = −31.6° ± 4.1°, corresponding to a proper motion amplitude of 5.05 ±0.35 μas yr−1. This is in good agreement with the acceleration expected from current models of the Galactic gravitational potential. We expect that future Gaia data releases will provide estimates of the acceleration with uncertainties substantially below 0.1 μas yr−1.

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“…Models with a lower mass get better χ 2 , but the mass in the fiducial model already strains the lower mass limit. The model mass of the cluster is 3.2 × 10 14 ( d 15.8Mpc )M while the virial theorem mass estimate is 6.0 ± 0.9 × 10 14 ( d 15.8Mpc )M (Kashibadze et al 2020). The H 0 = 77 cases reveal that higher H 0 can improves both cz and mass, but only slightly.…”

Section: Virgo Clustermentioning

confidence: 84%

Galaxy flows within 8,000 km/s from Numerical Action methods

Shaya,

Tully,

Pomarède

et al. 2022

Preprint

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The trajectories since z = 4 of systems of galaxies ('halos') with cz < 8, 000 km s −1 are found through Numerical Action reconstructions. A set of 9,719 halos from a 2MASS group catalog and Cosmicflows-3 catalogs are given attention. Present distances are adjusted to minimize departures from observed redshifts. For those with the most precisely determined distances, compromises are made between distance and redshift agreement. H 0 is varied from 69 to 77 km s −1 Mpc −1 with Ω m set by the baryon acoustic oscillation constraint from the Planck Satellite. A best fitting amplitude of the mass-to-light relation is found. A uniform density associated with the interhalo medium accounts for the matter not in halos. The solution paths provide the histories of the formation of the nearby large structures and depict how the voids emptied. Assuming no local over/underdensity, the best model has H 0 = 73 km s −1 Mpc −1 with nearly the same density arising from interhalo matter (IHM) as from halos. We examine local over/underdensities by varying the IHM density and find a valley of best fit models along H 0 = 73.0(1 + 0.165δ) km s −1 Mpc −1 . Friedmann models with distinct densities internal and external to the study region give a similar relationship. The fraction of matter in the IHM seen in n-body simulations roughly matches that in our H 0 = 72 scenario. Videos have been created to visualize the complexities of formation of large-scale structures. Standard n-body calculations starting from the first time-steps as tests of the NAM solutions, and continue until cosmic scale factor a = 2 provide glimpses into the future.

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Structure and kinematics of the Virgo cluster of galaxies

Cited by 49 publications

References 39 publications

Structures of Dwarf Satellites of Milky Way-like Galaxies: Morphology, Scaling Relations, and Intrinsic Shapes

Structures of Dwarf Satellites of Milky Way-like Galaxies: Morphology, Scaling Relations, and Intrinsic Shapes

GaiaEarly Data Release 3

Galaxy flows within 8,000 km/s from Numerical Action methods

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