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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 (August 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 (June 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 regions such as filaments, groups and clusters. The hot gas is only detectable via X-rays and the absorption of highly ionized species of heavy elements. The baryons in low density regions of space are excellent tracers of underlying dark matter. The evolution of the cosmic web indicates where to look for the baryons in collapsed objects but the overall inefficiency of galaxy formation has conspired to keep most baryons dark.

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Kraljic, Katarina, Christophe Pichon, Sandrine Codis, Clotilde Laigle, Romeel Davé, Yohan Dubois, Ho Seong Hwang, 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 (November 27, 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 mass: Less star forming and less rotation supported galaxies also tend to have higher connectivity. These results qualitatively hold both for observed and for virtual galaxies, and can be understood given that the cosmic web is the main source of fuel for galaxy growth. The simulations show the same trends at a fixed halo mass, suggesting that the geometry of filamentary infall impacts galaxy properties beyond the depth of the local potential well. Based on simulations, it is also found that active galactic nucleus feedback is key to reversing the relationship between stellar mass and connectivity at a fixed halo mass. Technically, connectivity is a practical observational proxy for past and present accretion (minor mergers or diffuse infall).

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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 (May 12, 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 a power spectrum of initial perturbations and an N-body simulation through to merger-history-tree based mass infall histories. The pipeline is built from well-established, free-licensed cosmological software packages, and aims at highly portable long-term reproducibility. We find that the elaphrocentric accelerations tending to oppose mass infall are modest. We do not find evidence of location in a void or elaphrocentric position weakening mass infall towards a galaxy. However, we find indirect evidence of voids influencing galaxy formation: while void galaxies are of lower mass compared to galaxies in high-density environments, their spin parameters are typically higher. For a fixed mass, the implied disc scale length would be greater. Tangential accelerations in voids are found to be high and might significantly contribute to the higher spin parameters. We find significantly later formation epochs for void galaxies; this should give lower matter densities and may imply lower surface densities of disc galaxies. Thus, void galaxies have higher spin parameters and later formation epochs; both are factors that may increase the probability of forming LSBGs in voids.

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5

Libeskind, Noam I. "The beaming of subhalo accretion." Proceedings of the International Astronomical Union 11, S308 (June 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 effectively universal in the sense that its always aligned with the axis of weakest collapse of the velocity shear tensor. It is the same shear tensor that dictates the structure of the cosmic web and hence the shear field emerges as the key factor that governs the local anisotropic pattern of structure formation. Since the small (sub-Mpc) scale is strongly correlated with the mid-range (∼ 10 Mpc) scale - a scale accessible by current surveys of peculiar velocities - it follows that findings presented here open a new window into the relation between the observed large scale structure unveiled by current surveys of peculiar velocities and the preferential infall direction of the Local Group. This may shed light on the unexpected alignments of dwarf galaxies seen in the Local Group.

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6

Hellwing, Wojciech A. "Dynamics of pairwise motions in the Cosmic Web." Proceedings of the International Astronomical Union 11, S308 (June 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 environment in which DM particle pairs are embedded. The pairwise flows are notably colder and have smaller mean magnitude in wall and voids, when compared to much denser environments of filaments and nodes. We discuss on our results, indicating that they are consistent with a simple theoretical predictions for pairwise motions as induced by gravitational instability mechanism. Our results indicate that the Cosmic Web elements are coherent dynamical entities rather than just temporal geometrical associations. In addition it should be possible to observationally test various Cosmic Web finding algorithms by segmenting available peculiar velocity data and studying resulting pairwise velocity statistics.

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7

Daddi, E., F. Valentino, R. M. Rich, J. D. Neill, M. Gronke, D. O’Sullivan, D. Elbaz, et al. "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 (May 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 accretion. The upper limits on active galactic nuclei activity and overall energetics favor gravity as the primary Lyα powering source and infall as the main source of gas flows to the system. Although interpretational difficulties remain, with outflows and likely also photoionization with ensuing recombination still playing a role, this finding provides arguably an ideal environment to quantitatively test models of cold gas accretion and galaxy feeding inside an actively star-forming massive halo at high redshift.

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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 (December 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 than today, and was thus able to keep the gas in the dwarfs warm and diffuse, were rapidly stripped of their baryons via ram pressure and tidal forces, producing very dark-matter-dominated objects with truncated star-formation histories, such as the Draco dSph. The low star-formation efficiency expected in such low-metallicity objects prior to their infall was crucial for keeping their disks gas dominated until stripping took over.Therefore gas stripping along with inefficient star-formation provides a new feedback mechanism, alternative to photoevaporation or supernovae feedback, playing a crucial role in dwarf galaxy formation and evolution. We also discuss how the ultra-faint dSphs belong to a different population of lower-mass dwarf satellites that were mostly shaped by reionization rather than by environmental mechanisms (“reionization fossils”). Finally, we scrutinize the various caveats in the current understanding of environmental effects as well as other recent ideas on the origin of Local Group dSphs.

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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 (August 14, 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 the baryon fraction of accreting matter, which we show to be heavily suppressed by stellar feedback in low-mass haloes, Mhalo ≲ 1011.5 M⊙. Breaking down accretion rates into first infall, recycled, transfer, and merger components, we show that baryons are much more likely to be smoothly accreted than to have originated from mergers when compared to DM, finding (averaged across halo mass) a merger contribution of $\approx 6{{\ \rm per\ cent}}$ for baryons, and $\approx 15{{\ \rm per\ cent}}$ for DM at z ≈ 0. We also show that the breakdown of inflow into different channels is strongly dependent on sub-grid physics, particularly the contribution of recycled accretion (accreting matter that has been previously ejected from progenitor haloes). Our findings highlight the dual role that baryonic feedback plays in regulating the evolution of galaxies and haloes: by (i) directly removing gas from haloes, and (ii) suppressing gas inflow to haloes.

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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 (August 6, 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 solutions, i.e. orbits that entered and left the MW dark matter halo in the past, and that velocities above $| \vec{u}_{\rm t}^{\rm GSR}| \ge 21^{+33}_{-21}\, {\rm km}\, {\rm s}^{\rm -1}$ result in wide-orbit backsplash solutions with a minimum pericentre range of $D_{\rm min} \ge 38^{+26}_{-16}\, {\rm kpc}$, which would allow this satellite to survive gas stripping and tidal disruption. Moreover, new proper motion estimates overlap with our orbital solution regions. We applied our method to other distant MW satellites, finding a range of gas stripped backsplash solutions for the gasless Cetus and Eridanus II, providing a possible explanation for their lack of cold gas, while only first infall solutions are found for the H i-rich Phoenix I. We also find that the cosmic expansion can delay their first pericentre passage when compared to the non-expanding scenario. This study explores the provenance of these distant dwarfs and provides constraints on the environmental and internal processes that shaped their evolution and current properties.

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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 (June 26, 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 text] and [Formula: see text] (Gyr), respectively. According to the constraint results on model parameters we discuss the evolutions of some cosmological quantities in structure formation, such as the density contrast and the growth variable. At last, the evolution of geometrical quantity is studied to distinguish the unified models of dark sectors with the cosmological constant model. It is shown that this unified model of dark matter and dark energy is attractive to interpret the accelerating universe.

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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 (May 2, 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 available, up to 0 < z < 10. Key findings include the following: galaxy assembly correlates strongly with halo assembly; quenching correlates strongly with halo mass; quenched fractions at fixed halo mass decrease with increasing redshift; massive quenched galaxies reside in higher-mass haloes than star-forming galaxies at fixed galaxy mass; star-forming and quenched galaxies’ star formation histories at fixed mass differ most at z < 0.5; satellites have large scatter in quenching time-scales after infall, and have modestly higher quenched fractions than central galaxies; Planck cosmologies result in up to 0.3 dex lower stellar – halo mass ratios at early times; and, none the less, stellar mass–halo mass ratios rise at z > 5. Also presented are revised stellar mass – halo mass relations for all, quenched, star-forming, central, and satellite galaxies; the dependence of star formation histories on halo mass, stellar mass, and galaxy SSFR; quenched fractions and quenching time-scale distributions for satellites; and predictions for higher-redshift galaxy correlation functions and weak lensing surface densities. The public data release (DR1) includes the massively parallel (>105 cores) implementation (the UniverseMachine), the newly compiled and remeasured observational data, derived galaxy formation constraints, and mock catalogues including lightcones.

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14

Goerdt, Tobias. "Cold streams: detectability, relation to structure and characteristics." Proceedings of the International Astronomical Union 10, S309 (July 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. The characteristics of the Ly alpha emission of our simulated galaxies are similar in luminosity, morphology and extent to the observed Ly alpha blobs, with distinct kinematic features. We analyse the characteristics of the cold streams in simulations and present scaling relations for the amount of infall, its velocity, distribution and its clumpiness and compare our findings with observations.

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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 (November 12, 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) the magnitudes of offsets from the galaxy centres are substantially larger in the simulation than in observations. We attribute the stalling of the infall and excessive offset magnitudes to the fact that dynamical friction from stars and dark matter is not modelled in the simulation, and hence provide a way to improve the BH dynamics of future simulations.

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Nasonova, O., I. Karachentsev, and V. Karachentseva. "Structure and kinematics of the Bootes filament." Proceedings of the International Astronomical Union 11, S308 (June 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 < 14h and some signs of outflow from the Local Void at RA > 17h. According to the galaxy grouping criterion, this complex contains the members of 13 groups, 11 pairs and 140 field galaxies. The most prominent group is dominated by NGC 5846. The Bootes filament contains the total stellar mass of 2.7 ×1012M⊙ and the total virial mass of 9.07×1013M⊙, having the average density of dark matter to be Ωm = 0.09, i.e. a factor three lower than the global cosmic value.

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17

DeYOUNG, TYCE. "NEUTRINO ASTRONOMY WITH ICECUBE." Modern Physics Letters A 24, no. 20 (June 28, 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 planned 86 strings operational. The new infill array known as Deep Core, which will extend IceCube's capabilities to energies as low as 10 GeV, is also described.

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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. Methods. Haloes and galaxies were identified and their kinematics computed using their dark matter and stellar particles respectively. Sub-haloes were discarded and galaxies lying within 5 Rvir of a given halo are matched to it. The filamentary structure of the cosmic web was extracted from the density field – smoothed over a 3 h−1 Mpc typical scale – as a network of contiguous segments. We then investigated the distribution function of relevant angles, most importantly the angle α between the central-to-satellite separation vector and the group’s nearest filament, aside with the angle between this same separation and the central minor axis. This allowed us to explore the correlations between filamentary infall, intra-cluster inspiralling and the resulting distribution of satellites around their central counterpart. Results. We find that, on average, satellites tend to be located on the galactic plane of the central object. This effect is detected for central galaxies with a stellar mass larger than 1010 M⊙ and found to be strongest for red passive galaxies, while blue galaxies exhibit a weaker trend. For galaxies with a minor axis parallel to the direction of the nearest filament, we find that the coplanarity is stronger in the vicinity of the central galaxy, and decreases when moving towards the outskirts of the host halo. By contrast, the spatial distribution of satellite galaxies relative to their closest filament follows the opposite trend: their tendency to align with them dominates at large distances from the central galaxy, and fades away in its vicinity. In that redshift range, we find hints that massive red centrals with a spin perpendicular to their filament also have corotating satellites well aligned with both the galactic plane and the filament. On the other hand, lower-mass blue centrals with a spin parallel to their filament have satellites flowing straight along this filament, and hence orthogonally to their galactic plane. The orbit of these satellites is then progressively bent towards a better alignment with the galactic plane as they penetrate the central region of their host halo. Conclusions. The kinematics previously described are consistent with satellite infall and spin build-up via quasi-polar flows, followed by a re-orientation of the spin of massive red galaxies through mergers.

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Diemand, Jürg, and Michael Kuhlen. "Infall Caustics in Dark Matter Halos?" Astrophysical Journal 680, no. 1 (May 19, 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 (March 21, 2007): 393–404. http://dx.doi.org/10.1111/j.1365-2966.2007.11439.x.

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

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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 (July 6, 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 anisotropy, suggesting that the local galaxy distribution is responsible for the microwave velocity. This will eventually provide the most reliable estimate of Ω, and is likely to result in a value somewhat larger than previous estimates on smaller scales. Study of the velocity field around large clusters in cosmological n-body experiments provides a useful guide for understanding the limitations of the spherically symmetric models of Virgocentric infall. We point out a number of biases that could affect the existing Virgocentric flow studies.

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Shi, Jingjing, Huiyuan Wang, H. J. Mo, Lizhi Xie, Xiaoyu Wang, Andrea Lapi, and Ravi K. Sheth. "Bimodal Formation Time Distribution for Infall Dark Matter Halos." Astrophysical Journal 857, no. 2 (April 24, 2018): 127. http://dx.doi.org/10.3847/1538-4357/aab775.

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Sellwood, J. A., and Stacy S. McGaugh. "The Compression of Dark Matter Halos by Baryonic Infall." Astrophysical Journal 634, no. 1 (November 20, 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 (December 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 (September 24, 2012): 507–34. http://dx.doi.org/10.1002/andp.201200212.

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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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Macciò, Andrea V., Daniel Huterer Prats, Keri L. Dixon, Tobias Buck, Stefan Waterval, Nikhil Arora, Stéphane Courteau, and Xi Kang. "Creating a galaxy lacking dark matter in a dark matter-dominated universe." Monthly Notices of the Royal Astronomical Society 501, no. 1 (December 2, 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 value of ∼25, as expected from numerical simulations and abundance matching techniques, to roughly unity as reported for NGC 1052-DF2 and NGC 1054-DF4. The stellar velocity dispersion drops from ∼30 $\, \rm km\, s^{-1}$ before infall to values as low as 6 ± 2 $\, \rm km\, s^{-1}$. These, and the half-light radius around 3 kpc, are in good agreement with observations from van Dokkum and collaborators. Our study shows that it is possible to create a galaxy without DM starting from typical dwarf galaxies formed in a DM-dominated universe, provided they live in a dense environment.

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Lokas, E. L. "Universal profile of dark matter haloes and the spherical infall model." Monthly Notices of the Royal Astronomical Society 311, no. 2 (January 15, 2000): 423–32. http://dx.doi.org/10.1046/j.1365-8711.2000.03082.x.

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Villanueva-Domingo, Pablo, Nickolay Y. Gnedin, and Olga Mena. "Warm Dark Matter and Cosmic Reionization." Astrophysical Journal 852, no. 2 (January 16, 2018): 139. http://dx.doi.org/10.3847/1538-4357/aa9ff5.

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

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Chen, Chuan-Ren, and Fuminobu Takahashi. "Cosmic rays from leptonic dark matter." Journal of Cosmology and Astroparticle Physics 2009, no. 02 (February 3, 2009): 004. http://dx.doi.org/10.1088/1475-7516/2009/02/004.

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Matsuda, Tomohiro. "Dark matter production from cosmic necklaces." Journal of Cosmology and Astroparticle Physics 2006, no. 04 (April 13, 2006): 005. http://dx.doi.org/10.1088/1475-7516/2006/04/005.

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

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

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Massey, Richard, Jason Rhodes, Richard Ellis, Nick Scoville, Alexie Leauthaud, Alexis Finoguenov, Peter Capak, et al. "Dark matter maps reveal cosmic scaffolding." Nature 445, no. 7125 (January 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 (April 17, 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 (November 1, 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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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 (August 30, 2018): 045. http://dx.doi.org/10.1088/1475-7516/2018/08/045.

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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 (October 10, 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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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 (June 28, 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 presence of local inhomogeneities. Constraints and observational tests of each of these cosmologies are proposed.

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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 (August 18, 2017): 3486–91. http://dx.doi.org/10.1093/mnras/stx2139.

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Roberts, Ian D., and Laura C. Parker. "‘Observing’ unrelaxed clusters in dark matter simulations." Monthly Notices of the Royal Astronomical Society 490, no. 1 (September 25, 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. Furthermore, we find that the fraction of non-Gaussian clusters increases strongly with cluster mass and modestly with redshift. For comparison, we also make use of three-dimensional information available in the simulations to explore the impact of projection on observational measurements. Differences between Gaussian and non-Gaussian clusters are much stronger when three-dimensional information is considered, which demonstrates that the strength of oberserved trends with cluster dynamics are diluted because observed velocity information is limited to one line-of-sight.

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PAVON, DIEGO, and WINFRIED ZIMDAHL. "DARK MATTER AND DISSIPATION." International Journal of Modern Physics D 03, no. 01 (March 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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Hagelin, John S., and Gordon L. Kane. "Cosmic ray antimatter from supersymmetric dark matter." Nuclear Physics B 263, no. 2 (January 1986): 399–412. http://dx.doi.org/10.1016/0550-3213(86)90123-9.

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

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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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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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