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Relevant bibliographies by topics / Cosmic infall

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Journal articles

Academic literature on the topic 'Cosmic infall'

Author: Grafiati

Published: 4 June 2021

Last updated: 6 February 2022

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Journal articles on the topic "Cosmic infall"

1

Jiang, I. G., and J. Binney. "Warps and cosmic infall." Monthly Notices of the Royal Astronomical Society 303, no. 1 (1999): L7—L10. http://dx.doi.org/10.1046/j.1365-8711.1999.02333.x.

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2

Shen, J., and J. A. Sellwood. "Galactic warps induced by cosmic infall." Monthly Notices of the Royal Astronomical Society 370, no. 1 (2006): 2–14. http://dx.doi.org/10.1111/j.1365-2966.2006.10477.x.

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3

Kraljic, Katarina, Christophe Pichon, Sandrine Codis, et al. "The impact of the connectivity of the cosmic web on the physical properties of galaxies at its nodes." Monthly Notices of the Royal Astronomical Society 491, no. 3 (2019): 4294–309. http://dx.doi.org/10.1093/mnras/stz3319.

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ABSTRACT We investigate the impact of the number of filaments connected to the nodes of the cosmic web on the physical properties of their galaxies using the Sloan Digital Sky Survey. We compare these measurements to the cosmological hydrodynamical simulations H orizon-(no)AGN and Simba. We find that more massive galaxies are more connected, in qualitative agreement with theoretical predictions and measurements in dark-matter-only simulations. The star formation activity and morphology of observed galaxies both display some dependence on the connectivity of the cosmic web at a fixed stellar ma

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4

Libeskind, Noam I. "The beaming of subhalo accretion." Proceedings of the International Astronomical Union 11, S308 (2014): 456–61. http://dx.doi.org/10.1017/s174392131601036x.

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AbstractWe examine the infall pattern of subhaloes onto hosts in the context of the large-scale structure. We find that the infall pattern is essentially driven by the shear tensor of the ambient velocity field. Dark matter subhaloes are preferentially accreted along the principal axis of the shear tensor which corresponds to the direction of weakest collapse. We examine the dependence of this preferential infall on subhalo mass, host halo mass and redshift. Although strongest for the most massive hosts and the most massive subhaloes at high redshift, the preferential infall of subhaloes is ef

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5

Fattahi, Azadeh, Alis J. Deason, Carlos S. Frenk, et al. "A tale of two populations: surviving and destroyed dwarf galaxies and the build-up of the Milky Way’s stellar halo." Monthly Notices of the Royal Astronomical Society 497, no. 4 (2020): 4459–71. http://dx.doi.org/10.1093/mnras/staa2221.

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ABSTRACT We use magnetohydrodynamical simulations of Milky Way-mass haloes from the Auriga project to investigate the properties of surviving and destroyed dwarf galaxies that are accreted by these haloes over cosmic time. We show that the combined luminosity function of surviving and destroyed dwarfs at infall is similar in the various Auriga haloes, and is dominated by the destroyed dwarfs. There is, however, a strong dependence on infall time: destroyed dwarfs typically have early infall times of less than 6 Gyr (since the big bang), whereas the majority of dwarfs accreted after 10 Gyr have

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6

Impey, Chris D. "Dim Baryons in the Cosmic Web." Proceedings of the International Astronomical Union 3, S244 (2007): 157–66. http://dx.doi.org/10.1017/s1743921307013956.

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AbstractThe distribution of baryons beyond galaxies is descibed. The majority of the baryons, which represent 4% of the cosmic mass and energy budget, lie far from individual galaxies in the diffuse intergalactic medium (IGM). Many of these baryons are in a warm phase that can be probed by quasar absorption in the Lyman-α line of hydrogen. The mature field of quasar spectroscopy can diagnose the location, physical state, metallicity, and general geometry of this gas, which is called the “cosmic web.” The remainder of the gas is kept very hot by infall and shocks and is mostly in higher density

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7

Peper, Marius, and Boudewijn F. Roukema. "The role of the elaphrocentre in void galaxy formation." Monthly Notices of the Royal Astronomical Society 505, no. 1 (2021): 1223–38. http://dx.doi.org/10.1093/mnras/stab1342.

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ABSTRACT Voids may affect galaxy formation via weakening mass infall or increasing disk sizes, which could potentially play a role in the formation of giant low surface brightness galaxies (LSBGs). If a dark matter halo forms at the potential hill corresponding to a void of the cosmic web, which we denote the ‘elaphrocentre’ in contrast to a barycentre, then the elaphrocentre should weaken the infall rate to the halo when compared to infall rates towards barycentres. We investigate this hypothesis numerically. We present a complete software pipeline to simulate galaxy formation, starting from

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8

Kashibadze, Olga G., and Igor D. Karachentsev. "Cosmic flow around local massive galaxies." Astronomy & Astrophysics 609 (December 22, 2017): A11. http://dx.doi.org/10.1051/0004-6361/201731645.

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Aims. We use accurate data on distances and radial velocities of galaxies around the Local Group, as well as around 14 other massive nearby groups, to estimate their radius of the zero-velocity surface, R0, which separates any group against the global cosmic expansion. Methods. Our R0 estimate was based on fitting the data to the velocity field expected from the spherical infall model, including effects of the cosmological constant. The reported uncertainties were derived by a Monte Carlo simulation. Results. Testing various assumptions about a location of the group barycentre, we found the op

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9

Hellwing, Wojciech A. "Dynamics of pairwise motions in the Cosmic Web." Proceedings of the International Astronomical Union 11, S308 (2014): 322–27. http://dx.doi.org/10.1017/s1743921316010085.

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AbstractWe present results of analysis of the dark matter (DM) pairwise velocity statistics in different Cosmic Web environments. We use the DM velocity and density field from the Millennium 2 simulation together with the NEXUS+ algorithm to segment the simulation volume into voxels uniquely identifying one of the four possible environments: nodes, filaments, walls or cosmic voids. We show that the PDFs of the mean infall velocities v12 as well as its spatial dependence together with the perpendicular and parallel velocity dispersions bear a significant signal of the large-scale structure envi

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10

Almeida, J. Sánchez, A. Olmo-García, B. G. Elmegreen, et al. "Gas accretion from the cosmic web feeding disk galaxies." Proceedings of the International Astronomical Union 11, S321 (2016): 208–10. http://dx.doi.org/10.1017/s1743921316008863.

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AbstractDisk galaxies in cosmological numerical simulations grow by accreting gas from the cosmic web. This gas reaches the external disk, and then spirals in dragged along by tidal forces and/or disk instabilities. The importance of gas infall is as clear from numerical simulations as it is obscure to observations. Extremely metal poor (XMP) galaxies seem to be the best example we have of the gas accretion process at work. They have large off-center starbursts which show significant metallicity drop compared with the host galaxy. This observation is naturally explained as a gas accretion even

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