Dark matter halo

Simulated dark matter halo from a cosmological N-body simulation

A dark matter halo is a hypothetical component of a galaxy that envelops the galactic disc and extends well beyond the edge of the visible galaxy. The halo's mass dominates the total mass. Since they consist of dark matter, halos cannot be observed directly, but their existence is inferred through their effects on the motions of stars and gas in galaxies. Dark matter halos play a key role in current models of galaxy formation and evolution.

Galaxy rotation curve for the Milky Way. Vertical axis is speed of rotation about the galactic center. Horizontal axis is distance from the galactic center. The sun is marked with a yellow ball. The observed curve of speed of rotation is blue. The predicted curve based upon stellar mass and gas in the Milky Way is red. Scatter in observations roughly indicated by gray bars. The difference is due to dark matter or perhaps a modification of the law of gravity.[1][2][3]

Rotation curves as evidence of a dark matter halo

The presence of dark matter (DM) in the halo is inferred from its gravitational effect on a spiral galaxy's rotation curve. Without large amounts of mass throughout the (roughly spherical) halo, the rotational velocity of the galaxy would decrease at large distances from the galactic center, just as the orbital speeds of the outer planets decrease with distance from the Sun. However, observations of spiral galaxies, particularly radio observations of line emission from neutral atomic hydrogen (known, in astronomical parlance, as HI), show that the rotation curve of most spiral galaxies flattens out, meaning that rotational velocities do not decrease with distance from the galactic center.[4] The absence of any visible matter to account for these observations implies either that unobserved ("dark") matter, first proposed by Ken Freeman in 1970, exist, or that the theory of motion under gravity (General Relativity) is incomplete. Freeman noticed that the expected decline in velocity was not present in NGC 300 nor M33, and considered an undetected mass to explain it. The DM Hypothesis has been reinforced by several studies.[5][6][7][8]

Formation and structure of dark matter halos

The formation of dark matter halos is believed to have played a major role in the early formation of galaxies. During the phase of time in the universe when galaxies were first formed, the temperature of the baryonic matter should have still been much too high for it to form gravitationally self-bound objects, thus requiring the prior formation of dark matter structure to add additional gravitational interactions. The current hypothesis for this is based on cold dark matter (CDM) and its formation into structure early in the universe.

The hypothesis for CDM structure formation begins with density perturbations in the Universe that grow linearly until they reach a critical density, after which they would stop expanding and collapse to form gravitationally bound dark matter halos. These halos would continue to grow in mass (and size), either through accretion of material from their immediate neighborhood, or by merging with other halos. Numerical simulations of CDM structure formation have been found to proceed as follows: A small volume with small perturbations initially expands with the expansion of the Universe. As time proceeds, small-scale perturbations grow and collapse to form small halos. At a later stage, these small halos merge to form a single virialized dark matter halo with an ellipsoidal shape, which reveals some substructure in the form of dark matter sub-halos.[9]

The use of CDM overcomes issues associated with the normal baryonic matter because it removes most of the thermal and radiative pressures that were preventing the collapse of the baryonic matter. The fact that the dark matter is cold compared to the baryonic matter allows the DM to form these initial, gravitationally bound clumps. Once these subhalos formed, their gravitational interaction with baryonic matter is enough to overcome the thermal energy, and allow it to collapse into the first stars and galaxies. Simulations of this early galaxy formation matches the structure observed by galactic surveys as well as observation of the Cosmic Microwave Background.[10]

Density profiles

A commonly used model for galactic dark matter halos is the pseudo-isothermal halo:[11]

where denotes the finite central density and the core radius. This provides a good fit to most rotation curve data. However, it cannot be a complete description, as the enclosed mass fails to converge to a finite value as the radius tends to infinity. The isothermal model is, at best, an approximation. Many effects may cause deviations from the profile predicted by this simple model. For example, (i) collapse may never reach an equilibrium state in the outer region of a dark matter halo, (ii) non-radial motion may be important, and (iii) mergers associated with the (hierarchical) formation of a halo may render the spherical-collapse model invalid.[12]

Numerical simulations of structure formation in an expanding universe lead to the theoretical prediction of the NFW (Navarro-Frenk-White) profile:[13]

where is a scale radius, is a characteristic (dimensionless) density, and = is the critical density for closure. The NFW profile is called 'universal' because it works for a large variety of halo masses, spanning four orders of magnitude, from individual galaxies to the halos of galaxy clusters. This profile has a finite gravitational potential even though the integrated mass still diverges logarithmically. It has become conventional to refer to the mass of a halo at a fiducial point that encloses an overdensity 200 times greater than the critical density of the universe, though mathematically the profile extends beyond this notational point. It was later deduced that the density profile depends on the environment, with the NFW appropriate only for isolated halos.[14] NFW halos generally provide a worse description of galaxy data than does the pseudo-isothermal profile, leading to the cuspy halo problem.

Higher resolution computer simulations are better described by the Einasto profile:[15]

where r is the spatial (i.e., not projected) radius. The term is a function of n such that is the density at the radius that defines a volume containing half of the total mass. While the addition of a third parameter provides a slightly improved description of the results from numerical simulations, it is not observationally distinguishable from the 2 parameter NFW halo,[16] and does nothing to alleviate the cuspy halo problem.

Shape

The collapse of overdensities in the cosmic density field is generally aspherical. So, there is no reason to expect the resulting halos to be spherical. Even the earliest simulations of structure formation in a CDM universe emphasized that the halos are substantially flattened.[17] Subsequent work has shown that halo equidensity surfaces can be described by ellipsoids characterized by the lengths of their axes.[18]

Because of uncertainties in both the data and the model predictions, it is still unclear whether the halo shapes inferred from observations are consistent with the predictions of ΛCDM cosmology.

Halo substructure

Up until the end of the 1990s, numerical simulations of halo formation revealed little substructure. With increasing computing power and better algorithms, it became possible to use greater numbers of particles and obtain better resolution. Substantial amounts of substructure are now expected.[19][20][21] When a small halo merges with a significantly larger halo it becomes a subhalo orbiting within the potential well of its host. As it orbits, it is subjected to strong tidal forces from the host, which cause it to lose mass. In addition the orbit itself evolves as the subhalo is subjected to dynamical friction which causes it to lose energy and angular momentum to the dark matter particles of its host. Whether a subhalo survives as a self-bound entity depends on its mass, density profile, and its orbit.[22]

Angular momentum

As originally pointed out by Hoyle[23] and first demonstrated using numerical simulations by Efstathiou & Jones,[24] asymmetric collapse in an expanding universe produces objects with significant angular momentum.

Numerical simulations have shown that the spin parameter distribution for halos formed by dissipation-less hierarchical clustering is well fit by a log-normal distribution, the median and width of which depend only weakly on halo mass, redshift, and cosmology:[25]

with and . At all halo masses, there is a marked tendency for halos with higher spin to be in denser regions and thus to be more strongly clustered.[26]

Theories about the nature of dark matter

The nature of dark matter in the galactic halos of spiral galaxies is still undetermined, but there are two popular theories: either the halo is composed of weakly interacting elementary particles known as WIMPs, or it is composed of a number of small, dark bodies known as MACHOs. MACHOs, an acronym for massive compact halo objects, would be composed of “ordinary” matter that simply does not emit easily detectable radiation. The reliance of modern astronomy on detecting electromagnetic radiation would render dim, but massive objects, nearly undetectable. A wide range of possible MACHO candidates have been suggested, encompassing everything from black holes to very dim dwarf stars. Despite being too dim to detect directly via electromagnetic telescopes, MACHOs would necessarily interact gravitationally, as described by general relativity. The preferred method for searching for MACHOs in the halo of our own galaxy has been to look for microlensing events. Gravitational microlensing occurs when two stars fall on a common line of sight, rendering the far star obscured by the near one. However, as light from the far star passes through the gravitational well of the near star the light bends, creating an Einstein Halo. In a microlensing event, the halo is so small that it is optically indistinguishable from the star. The overall effect is to simply make the star appear brighter. The EROS and MACHO projects search of MACHOs in the halo by observing stars in the small and large Magellanic clouds. If a MACHO existed in the halo along the line of sight of stars in the cloud, the lensing would brighten it from that orientation as opposed to others. The magnitude and number (or lack of) lensing events can be used to place bounds on the masses of any MACHOs which might be in the halo. The two projects initially were able to place a very strict limit on MACHOS in the range of concluding that such light mass MACHOs could, at most, only constitute 10% of the accepted mass of our dark matter halo.[27] Two years later, the EROS2 project extended this limit, concluding that any MACHO less than a single solar mass could not make up a significant part of the halo.[28] The two collaborations were able to extend this to a rather large window, ruling out any MACHO in the window. The final window of extremely heavy MACHOs above were ruled out by comparing Monte Carlo method simulations to observed distributions,[29] which the authors indicate as “The End of the MACHO Era”. Extremely light MACHOs less than the current limit are also not a viable possibility, as such light mass objects would not have survived on the timescale that it would take for the galaxy to form.[30]

Milky Way dark matter halo

The visible disk of the Milky Way Galaxy is embedded in a much larger, roughly spherical halo of dark matter. The dark matter density drops off with distance from the galactic center. It is now believed that about 95% of the Galaxy is composed of dark matter, a type of matter that does not seem to interact with the rest of the Galaxy's matter and energy in any way except through gravity. The luminous matter makes up approximately 9 x 1010 solar masses. The dark matter halo is likely to include around 6 x 1011 to 3 x 1012 solar masses of dark matter.[31][32]

See also

References

  1. ↑ Peter Schneider (2006). Extragalactic Astronomy and Cosmology. Springer. p. 4, Figure 1.4. ISBN 3-540-33174-3.
  2. ↑ Theo Koupelis; Karl F Kuhn (2007). In Quest of the Universe. Jones & Bartlett Publishers. p. 492; Figure 16-13. ISBN 0-7637-4387-9.
  3. ↑ Mark H. Jones; Robert J. Lambourne; David John Adams (2004). An Introduction to Galaxies and Cosmology. Cambridge University Press. p. 21; Figure 1.13. ISBN 0-521-54623-0.
  4. ↑ Bosma, A. (1978), Phy. D. Thesis, Univ. of Groningen
  5. ↑ Freeman, K.C. (1970), Astrophys. J. 160,881
  6. ↑ Rubin, V. C., Ford, W. K. and Thonnard, N. (1980), Astrophys. J. 238,471
  7. ↑ Bregman, K. (1987), Ph. Thesis, Univ. Groningen
  8. ↑ Broeils, A. H. (1992), Astron. Astrophys. J. 256, 19
  9. ↑ Houjun Mo, Frank Van den Bosch, S. White (2010, Galaxy formation and Evolution, Cambridge University Press.
  10. ↑ Springel, Boker, et el, (2005), Nature, 629, 636
  11. ↑ Gunn, J. and Gott, J.R. (1972), Astrophys. J. 176.1
  12. ↑ Houjun Mo, Frank Van den Bosch, S. White (2010), Galaxy formation and Evolution, Cambridge University Press.
  13. ↑ Navarro, J. et al. (1997), A Universal Density Profile from Hierarchical Clustering
  14. ↑ Avila-Reese, V., Firmani, C. and Hernandez, X. (1998), Astrophys. J. 505, 37.
  15. ↑ Merritt, D. et al. (2006), Empirical Models for Dark Matter Halos. I. Nonparametric Construction of Density Profiles and Comparison with Parametric Models
  16. ↑ McGaugh, S. "et al." (2007), The Rotation Velocity Attributable to Dark Matter at Intermediate Radii in Disk Galaxies
  17. ↑ Davis, M., Efstathiou, G., Frenk, C. S., White, S. D. M. (1985), ApJ. 292, 371
  18. ↑ Franx, M., Illingworth, G., de Zeeuw, T. (1991), ApJ., 383, 112
  19. ↑ Klypin, A., Gotlöber, S., Kravtsov, A. V., Khokhlov, A. M. (1999), ApJ., 516,530
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  21. ↑ Springel, V., Wang, J., Vogelsberger, M., et al. (2008), MNRAS, 391,1685
  22. ↑ Houjun Mo, Frank Van den Bosch, S. White (2010), Galaxy formation and Evolution, Cambridge University Press
  23. ↑ Hoyle, F. (1949), Problems of Cosmical Aerodynamics, Central Air Documents Office, Dayton.
  24. ↑ Efstathiou, G., Jones, B. J. T. (1979), MNRAS, 186, 133
  25. ↑ Maccio, A. V., Dutton, A. A., van den Bosch, F. C., et al. (2007), MNRAS, 378, 55
  26. ↑ Gao, L., White, S. D. M. (2007), MNRAS, 377, L5
  27. ↑ Alcock, C.; Allsman, R. A.; Alves, D.; Ansari, R.; Aubourg, É; Axelrod, T. S.; Bareyre, P.; Beaulieu, J.-Ph; Becker, A. C. (1998-01-01). "EROS and MACHO Combined Limits on Planetary-Mass Dark Matter in the Galactic Halo". The Astrophysical Journal Letters. 499 (1): L9. Bibcode:1998ApJ...499L...9A. ISSN 1538-4357. arXiv:astro-ph/9803082 Freely accessible. doi:10.1086/311355.
  28. ↑ Lasserre, T.; Collaboration, EROS (2000-02-11). "Not enough stellar Mass Machos in the Galactic Halo". Astronomy and Astrophysics Letters. 355: L39–L42. Bibcode:2000A&A...355L..39L. arXiv:astro-ph/0002253 Freely accessible.
  29. ↑ Yoo, Jaiyul; Chanamé, Julio; Gould, Andrew (2004-01-01). "The End of the MACHO Era: Limits on Halo Dark Matter from Stellar Halo Wide Binaries". The Astrophysical Journal. 601 (1): 311. Bibcode:2004ApJ...601..311Y. ISSN 0004-637X. arXiv:astro-ph/0307437 Freely accessible. doi:10.1086/380562.
  30. ↑ de Rujula, A.; Jetzer, P.; Masso, E. (1992-02-01). "On the Nature of the Dark Halo of Our Galaxy". Astronomy and Astrophysics. 254: 99. Bibcode:1992A&A...254...99D. ISSN 0004-6361.
  31. ↑ Battaglia et al. (2005), The radial velocity dispersion profile of the Galactic halo: constraining the density profile of the dark halo of the Milky Way
  32. ↑ Kafle, P.R.; Sharma, S.; Lewis, G.F.; Bland-Hawthorn, J. (2014). "On the Shoulders of Giants: Properties of the Stellar Halo and the Milky Way Mass Distribution". The Astrophysical Journal. 794 (1): 17. Bibcode:2014ApJ...794...59K. arXiv:1408.1787 Freely accessible. doi:10.1088/0004-637X/794/1/59.

Further reading

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