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Journal articles on the topic 'Dark matter; Cosmic infall'

Author: Grafiati

Published: 4 June 2021

Last updated: 11 February 2022

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1

Aubert, D., C. Pichon, and S. Colombi. "The origin and implications of dark matter anisotropic cosmic infall on ≈L★haloes." Monthly Notices of the Royal Astronomical Society 352, no. 2 (2004): 376–98. http://dx.doi.org/10.1111/j.1365-2966.2004.07883.x.

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2

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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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

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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5

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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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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Daddi, E., F. Valentino, R. M. Rich та ін. "Three Lyman-α-emitting filaments converging to a massive galaxy group at z = 2.91: discussing the case for cold gas infall". Astronomy & Astrophysics 649 (травень 2021): A78. http://dx.doi.org/10.1051/0004-6361/202038700.

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We have discovered a 300 kpc-wide giant Lyman-α (Lyα) nebula centered on the massive galaxy group RO-1001 at z = 2.91 in the Cosmic Evolution Survey field. Keck Cosmic Web Imager observations reveal three cold gas filaments converging into the center of the potential well of its ∼4 × 1013 M⊙ dark matter halo, hosting 1200 M⊙ yr−1 of star formation as probed by Atacama Large Millimeter Array and NOrthern Extended Millimeter Array observations. The nebula morphological and kinematics properties and the prevalence of blueshifted components in the Lyα spectra are consistent with a scenario of gas

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8

ALIMI, JEAN-MICHEL, and ANDRÉ FÜZFA. "IS DARK ENERGY ABNORMALLY WEIGHTING?" International Journal of Modern Physics D 16, no. 12b (2007): 2587–92. http://dx.doi.org/10.1142/s0218271807011206.

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We investigate the possibility that dark energy does not couple to gravitation in the same way as ordinary matter, yielding a violation of the weak and strong equivalence principles on cosmological scales. We build a transient mechanism in which gravitation is pushed away from general relativity (GR) by a Born–Infeld (BI) gauge interaction acting as an "abnormally weighting (dark) energy" (AWE). This mechanism accounts for the Hubble diagram of far-away supernovae by cosmic acceleration and time variation of the gravitational constant while accounting naturally for the present tests on GR.

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9

Mayer, Lucio. "Environmental Mechanisms Shaping the Nature of Dwarf Spheroidal Galaxies: The View of Computer Simulations." Advances in Astronomy 2010 (2010): 1–21. http://dx.doi.org/10.1155/2010/278434.

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We review numerical works carried out over the last decade on the role of environmental mechanisms in shaping nature of the faintest galaxies known, dwarf spheroidals (dSphs). The combination of tidally induced morphological transformation, termed tidal stirring, with mass loss due to tidal and ram-pressure stripping aided by heating due to the cosmic ionizing background can turn late-type dwarfs resembling present-day dIrrs into classic dSphs. The time of infall into the primary halo is shown to be a key parameter. Dwarfs accreting at when the cosmic ultraviolet ionizing flux was much higher

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10

Wright, Ruby J., Claudia del P. Lagos, Chris Power, and Peter D. Mitchell. "The impact of stellar and AGN feedback on halo-scale baryonic and dark matter accretion in the eagle simulations." Monthly Notices of the Royal Astronomical Society 498, no. 2 (2020): 1668–92. http://dx.doi.org/10.1093/mnras/staa2359.

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ABSTRACT We use the eagle suite of hydrodynamical simulations to analyse accretion rates (and the breakdown of their constituent channels) on to haloes over cosmic time, comparing the behaviour of baryons and dark matter (DM). We also investigate the influence of sub-grid baryon physics on halo-scale inflow, specifically the consequences of modelling radiative cooling, as well as feedback from stars and active galactic nuclei (AGNs). We find that variations in halo baryon fractions at fixed mass (particularly their circumgalactic medium gas content) are very well correlated with variations in

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11

Blaña, Matías, Andreas Burkert, Michael Fellhauer, Marc Schartmann, and Christian Alig. "Dwarfs in the Milky Way halo outer rim: first infall or backsplash satellites?" Monthly Notices of the Royal Astronomical Society 497, no. 3 (2020): 3601–22. http://dx.doi.org/10.1093/mnras/staa2153.

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ABSTRACT Leo T is a gas-rich dwarf located at $414\, {\rm kpc}$ (1.4Rvir) distance from the Milky Way (MW) and it is currently assumed to be on its first approach. Here, we present an analysis of orbits calculated backwards in time for the dwarf with our new code delorean, exploring a range of systematic uncertainties, e.g. MW virial mass and accretion, M31 potential, and cosmic expansion. We discover that orbits with tangential velocities in the Galactic standard-of-rest frame lower than $| \vec{u}_{\rm t}^{\rm GSR}| \le 63^{+47}_{-39}\, {\rm km}\, {\rm s}^{\rm -1}$ result in backsplash solut

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12

LU, JIANBO, LIXIN XU, YABO WU, MOLIN LIU, and TIANQIANG LI. "STUDY ON A UNIFIED MODEL OF DARK MATTER AND DARK ENERGY FROM DBI THEORY." International Journal of Modern Physics D 22, no. 09 (2013): 1350059. http://dx.doi.org/10.1142/s0218271813500594.

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In this paper, we study a unified model of dark matter and dark energy obtained from Dirac–Born–Infeld (DBI) action in string theory. Two accelerated expansions in universe can be unified in this action. By using the Markov Chain Monte Carlo method, we fit the current observational data to constrain the model parameters in this unified model, where various density parameters as model parameters are included, and their constraint values are: [Formula: see text], [Formula: see text], [Formula: see text] and [Formula: see text]. In addition, the Hubble constant and cosmic age are [Formula: see te

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13

Behroozi, Peter, Risa H. Wechsler, Andrew P. Hearin, and Charlie Conroy. "UniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10." Monthly Notices of the Royal Astronomical Society 488, no. 3 (2019): 3143–94. http://dx.doi.org/10.1093/mnras/stz1182.

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ABSTRACTWe present a method to flexibly and self-consistently determine individual galaxies’ star formation rates (SFRs) from their host haloes’ potential well depths, assembly histories, and redshifts. The method is constrained by galaxies’ observed stellar mass functions, SFRs (specific and cosmic), quenched fractions, ultraviolet (UV) luminosity functions, UV–stellar mass relations, IRX–UV relations, auto- and cross-correlation functions (including quenched and star-forming subsamples), and quenching dependence on environment; each observable is reproduced over the full redshift range avail

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14

Goerdt, Tobias. "Cold streams: detectability, relation to structure and characteristics." Proceedings of the International Astronomical Union 10, S309 (2014): 269–72. http://dx.doi.org/10.1017/s1743921314009843.

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AbstractCold gas streaming along the dark-matter filaments of the cosmic web is predicted to be the major provider of resources for disc buildup and star formation in massive galaxies in the early universe. We use hydrodynamical simulations to study to what extent these cold streams are traceable in the extended circum-galactic environment of galaxies via Ly alpha emission, Ly alpha absorption and selected low ionisation metal absorption lines. We predict the strength of the absorption signal produced by the streams and find that it is consistent with observations in high redshift galaxies. Th

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15

Bartlett, Deaglan J., Harry Desmond, Julien Devriendt, Pedro G. Ferreira, and Adrianne Slyz. "Spatially offset black holes in the Horizon-AGN simulation and comparison to observations." Monthly Notices of the Royal Astronomical Society 500, no. 4 (2020): 4639–57. http://dx.doi.org/10.1093/mnras/staa3516.

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ABSTRACT We study the displacements between the centres of galaxies and their supermassive black holes (BHs) in the cosmological hydrodynamical simulation Horizon-AGN, and in a variety of observations from the literature. The BHs in Horizon-AGN feel a subgrid dynamical friction force, sourced by the surrounding gas, which prevents recoiling BHs being ejected from the galaxy. We find that (i) the fraction of spatially offset BHs increases with cosmic time, (ii) BHs live on prograde orbits in the plane of the galaxy with an orbital radius that decays with time but stalls near z = 0, and (iii) th

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16

Nasonova, O., I. Karachentsev, and V. Karachentseva. "Structure and kinematics of the Bootes filament." Proceedings of the International Astronomical Union 11, S308 (2014): 187–92. http://dx.doi.org/10.1017/s1743921316009820.

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AbstractBootes filament of galaxies is a dispersed chain of groups residing on sky between the Local Void and the Virgo cluster. We consider a sample of 361 galaxies inside the sky area of RA = 13h0...18h.5 and Dec = .5°... + 10° with radial velocities VLG < 2000 km/s to clarify its structure and kinematics. In this region, 161 galaxies have individual distance estimates. We use these data to draw the Hubble relation for galaxy groups, pairs as well as the field galaxies, and to examine the galaxy distribution on peculiar velocities. Our analysis exposes the known Virgo-centric infall at RA

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17

DeYOUNG, TYCE. "NEUTRINO ASTRONOMY WITH ICECUBE." Modern Physics Letters A 24, no. 20 (2009): 1543–57. http://dx.doi.org/10.1142/s0217732309031417.

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IceCube is a kilometer-scale high energy neutrino telescope under construction at the South Pole, a second-generation instrument expanding the capabilities of the AMANDA telescope. The scientific portfolio of IceCube includes the detection of neutrinos from astrophysical objects such as the sources of the cosmic rays, the search for dark matter, and fundamental physics using a very large data set of atmospheric neutrinos. The design and status of IceCube are briefly reviewed, followed by a summary of results to date from AMANDA and initial IceCube results from the 2007 run, with 22 of a planne

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18

Welker, C., Y. Dubois, C. Pichon, J. Devriendt, and N. E. Chisari. "Caught in the rhythm." Astronomy & Astrophysics 613 (May 2018): A4. http://dx.doi.org/10.1051/0004-6361/201629007.

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Context. The anisotropic distribution of satellites around the central galaxy of their host halo is both well-documented in observations and predicted by the ΛCDM model. However its amplitude, direction and possible biases associated to the specific dynamics of such satellite galaxies are still highly debated. Aims. Using the cosmological hydrodynamics simulation Horizon-AGN, we aim to quantify the anisotropy of the spatial distribution of satellite galaxies relative to their central counterpart and explore its connexion to the local cosmic web, in the redshift range between 0.3 and 0.8. Metho

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19

Diemand, Jürg, and Michael Kuhlen. "Infall Caustics in Dark Matter Halos?" Astrophysical Journal 680, no. 1 (2008): L25—L28. http://dx.doi.org/10.1086/589688.

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20

Ascasibar, Yago, Yehuda Hoffman, and Stefan Gottlöber. "Secondary infall and dark matter haloes." Monthly Notices of the Royal Astronomical Society 376, no. 1 (2007): 393–404. http://dx.doi.org/10.1111/j.1365-2966.2007.11439.x.

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21

Dolag, K., A. D. Dolgov, and I. I. Tkachev. "Resolving infall caustics in dark matter halos." JETP Letters 96, no. 12 (2013): 754–58. http://dx.doi.org/10.1134/s0021364012240022.

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22

Cole, David R., Walter Dehnen, and Mark I. Wilkinson. "Weakening dark matter cusps by clumpy baryonic infall." Monthly Notices of the Royal Astronomical Society 416, no. 2 (2011): 1118–34. http://dx.doi.org/10.1111/j.1365-2966.2011.19110.x.

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23

Davis, Marc. "Evidence for Dark Matter in Galactic Systems." Symposium - International Astronomical Union 117 (1987): 97–110. http://dx.doi.org/10.1017/s0074180900149964.

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The evidence for dark matter in binaries and groups of galaxies is very strong, and is seen in all recent observational studies. Measurements of mass in galactic systems is possible on scales ranging from 50 kpc using virial analysis of binary galaxies to 15 Mpc using Virgocentric infall analysis. The Ω estimates derived from these studies are generally consistent with Ω < 0.2, with a fairly weak trend toward larger Ω estimates on larger scales. However, measurements of the galaxy distribution in the IRAS catalog yields a dipole anisotropy consistent in direction with the microwave dipole a

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24

Shi, Jingjing, Huiyuan Wang, H. J. Mo, et al. "Bimodal Formation Time Distribution for Infall Dark Matter Halos." Astrophysical Journal 857, no. 2 (2018): 127. http://dx.doi.org/10.3847/1538-4357/aab775.

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25

Sellwood, J. A., and Stacy S. McGaugh. "The Compression of Dark Matter Halos by Baryonic Infall." Astrophysical Journal 634, no. 1 (2005): 70–76. http://dx.doi.org/10.1086/491731.

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26

Primack, J. R., D. Seckel, and B. Sadoulet. "Detection of Cosmic Dark Matter." Annual Review of Nuclear and Particle Science 38, no. 1 (1988): 751–807. http://dx.doi.org/10.1146/annurev.ns.38.120188.003535.

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27

Frenk, C. S., and S. D. M. White. "Dark matter and cosmic structure." Annalen der Physik 524, no. 9-10 (2012): 507–34. http://dx.doi.org/10.1002/andp.201200212.

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28

Blumenthal, G. R., S. M. Faber, R. Flores, and J. R. Primack. "Contraction of dark matter galactic halos due to baryonic infall." Astrophysical Journal 301 (February 1986): 27. http://dx.doi.org/10.1086/163867.

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29

Macciò, Andrea V., Daniel Huterer Prats, Keri L. Dixon, et al. "Creating a galaxy lacking dark matter in a dark matter-dominated universe." Monthly Notices of the Royal Astronomical Society 501, no. 1 (2020): 693–700. http://dx.doi.org/10.1093/mnras/staa3716.

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ABSTRACT We use hydrodynamical cosmological simulations to show that it is possible to create, via tidal interactions, galaxies lacking dark matter (DM) in a DM-dominated universe. We select dwarf galaxies from the NIHAO project, obtained in the standard cold dark matter model and use them as initial conditions for simulations of satellite–central interactions. After just one pericentric passage on an orbit with a strong radial component, NIHAO dwarf galaxies can lose up to 80 per cent of their DM content, but, most interestingly, their central (≈8 kpc) DM-to-stellar mass ratio changes from a

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30

Lokas, E. L. "Universal profile of dark matter haloes and the spherical infall model." Monthly Notices of the Royal Astronomical Society 311, no. 2 (2000): 423–32. http://dx.doi.org/10.1046/j.1365-8711.2000.03082.x.

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31

Villanueva-Domingo, Pablo, Nickolay Y. Gnedin, and Olga Mena. "Warm Dark Matter and Cosmic Reionization." Astrophysical Journal 852, no. 2 (2018): 139. http://dx.doi.org/10.3847/1538-4357/aa9ff5.

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32

Ananthaswamy, Anil. "Dark matter born in cosmic twists." New Scientist 237, no. 3165 (2018): 8. http://dx.doi.org/10.1016/s0262-4079(18)30285-9.

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33

Chen, Chuan-Ren, and Fuminobu Takahashi. "Cosmic rays from leptonic dark matter." Journal of Cosmology and Astroparticle Physics 2009, no. 02 (2009): 004. http://dx.doi.org/10.1088/1475-7516/2009/02/004.

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34

Matsuda, Tomohiro. "Dark matter production from cosmic necklaces." Journal of Cosmology and Astroparticle Physics 2006, no. 04 (2006): 005. http://dx.doi.org/10.1088/1475-7516/2006/04/005.

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35

Grimani, C. "Cosmic-ray observations and dark matter." Nuclear Physics B - Proceedings Supplements 85, no. 1-3 (2000): 298–302. http://dx.doi.org/10.1016/s0920-5632(00)00521-1.

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36

Salati, P. "Cosmic rays from dark matter annihilations." Nuclear Physics B - Proceedings Supplements 87, no. 1-3 (2000): 366–76. http://dx.doi.org/10.1016/s0920-5632(00)00699-x.

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37

Massey, Richard, Jason Rhodes, Richard Ellis, et al. "Dark matter maps reveal cosmic scaffolding." Nature 445, no. 7125 (2007): 286–90. http://dx.doi.org/10.1038/nature05497.

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38

Tenkanen, Tommi. "Cosmic inflation constrains scalar dark matter." Cogent Physics 2, no. 1 (2015): 1029845. http://dx.doi.org/10.1080/23311940.2015.1029845.

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39

Liang, Bin. "The Dark Matter and Dark Energy in Cosmic Evolution." Applied Physics Research 9, no. 6 (2017): 14. http://dx.doi.org/10.5539/apr.v9n6p14.

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This article is on an in-depth study of the relationship between the dark matter, dark energy, radiation field and gravitation field, based on the standard cosmic model and the principle that dark energy is originated from the destructive interference of electromagnetic radiation field. It explains the dynamic mechanism of cosmic expansion and contraction, and calculates the densities of dark matter, dark energy, radiation field and gravitation field.

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40

Das, Subinoy, Rajesh Mondal, Vikram Rentala, and Srikanth Suresh. "On dark matter-dark radiation interaction and cosmic reionization." Journal of Cosmology and Astroparticle Physics 2018, no. 08 (2018): 045. http://dx.doi.org/10.1088/1475-7516/2018/08/045.

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41

SRIVASTAVA, S. K., and K. P. SINHA. "RICCION AS A COSMIC DARK MATTER CANDIDATE AND LATE COSMIC ACCELERATION." Modern Physics Letters A 23, no. 31 (2008): 2681–89. http://dx.doi.org/10.1142/s0217732308026352.

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In the past few years, a possibility is investigated, where curvature itself behaves as a source of dark energy. So, it is natural to think whether curvature can produce dark matter too. It is found that, at classical level, higher-derivative gravity yields curvature inspired particles namely riccions.31 Here, it is probed whether riccion can be a possible source of dark matter. Further, it is found that the late universe accelerates. Here, it is interesting to see that acceleration is obtained from curvature without using any dark energy source of exotic matter.

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42

MATHEWS, GRANT J., K. ICHIKI, T. KAJINO, N. Q. LAN, and X. ZHAO. "ALTERNATIVE UNIFIED VIEWS ON DARK MATTER AND DARK ENERGY." Modern Physics Letters A 23, no. 17n20 (2008): 1372–83. http://dx.doi.org/10.1142/s0217732308027746.

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The simple fact that the present closure contributions in dark matter and dark energy are nearly equal begs the question as to whether they could be different aspects of the same physical phenomenon. Here, we review constraints several postulates as to how this coincidence could be achieved. These include: 1) The possibility that the dark matter decays producing a bulk viscosity in the cosmic fluid; 2) cosmic acceleration produced by the inflow of dark matter from a bulk dimension in brane-world cosmology; and 3) The possibility of relativistic corrections to the Friedmann equation from the pr

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43

Albæk, L., S. H. Hansen, D. Martizzi, B. Moore, and R. Teyssier. "Infall near clusters of galaxies: comparing gas and dark matter velocity profiles." Monthly Notices of the Royal Astronomical Society 472, no. 3 (2017): 3486–91. http://dx.doi.org/10.1093/mnras/stx2139.

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44

Roberts, Ian D., and Laura C. Parker. "‘Observing’ unrelaxed clusters in dark matter simulations." Monthly Notices of the Royal Astronomical Society 490, no. 1 (2019): 773–83. http://dx.doi.org/10.1093/mnras/stz2666.

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ABSTRACT We present a detailed study of relaxed and unrelaxed galaxy clusters in a large dark matter only simulation. Recent work has demonstrated clear differences between the galaxy populations in clusters that have Gaussian velocity distributions (relaxed) compared to those that do not (unrelaxed). To directly compare with observations, we identify unrelaxed clusters in the simulations using one-dimensional velocity distributions. We show that non-Gaussian clusters have had recent major mergers and enhanced rates of galaxy infall relative to systems with Gaussian velocity profiles. Furtherm

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45

PAVON, DIEGO, and WINFRIED ZIMDAHL. "DARK MATTER AND DISSIPATION." International Journal of Modern Physics D 03, no. 01 (1994): 245–48. http://dx.doi.org/10.1142/s0218271894000381.

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The uncertainty about the current values of the observational parameters leaves ample room for a bulk dissipative stress on cosmic scales which, we argue, may be ascribed to the presence of dark matter. As a byproduct the constraint 2q0<Ω0 is obtained.

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46

Hagelin, John S., and Gordon L. Kane. "Cosmic ray antimatter from supersymmetric dark matter." Nuclear Physics B 263, no. 2 (1986): 399–412. http://dx.doi.org/10.1016/0550-3213(86)90123-9.

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47

Fabbri, R. "Tests for cosmic dark matter from COBE." Astroparticle Physics 6, no. 1 (1996): 25–34. http://dx.doi.org/10.1016/s0927-6505(96)00039-4.

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48

Lineros, Roberto A. "Dark Matter detection via lepton cosmic rays." Journal of Physics: Conference Series 259 (November 1, 2010): 012101. http://dx.doi.org/10.1088/1742-6596/259/1/012101.

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49

Cirelli, Marco. "Dark matter indirect searches: charged cosmic rays." Journal of Physics: Conference Series 718 (May 2016): 022005. http://dx.doi.org/10.1088/1742-6596/718/2/022005.

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von Doetinchem, Philip. "Dark matter identification with cosmic-ray antideuterons." Journal of Physics: Conference Series 718 (May 2016): 042061. http://dx.doi.org/10.1088/1742-6596/718/4/042061.

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