Advances in Astronomy

Volume 2009, Article ID 752439, 9 pages

http://dx.doi.org/10.1155/2009/752439

## Modified Newtonian Dynamics: A Falsification of Cold Dark Matter

Kapteyn Astronomical Institute, University of Groningen, 9700 AV Groningen, The Netherlands

Received 24 February 2009; Accepted 11 August 2009

Academic Editor: Kenneth Freeman

Copyright © 2009 R. H. Sanders. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

#### Abstract

The only viable alternative to dark matter is one in which Newtonian dynamics or gravity breaks down in the limit of low accelerations, as in modified Newtonian dynamics (MONDs). This hypothesis, suggested by Milgrom, has been successful in explaining systematic properties of spiral and elliptical galaxies and predicting in detail the observed rotation curves of spiral galaxies with only one additional parameter—a critical acceleration which is on the order of the cosmologically interesting value of . MOND may be viewed as an algorithm for calculating the distribution of force in an astronomical object from the observed distribution of baryonic matter. The fact that it works very well on the scale of galaxies is problematic for cold dark matter (CDM). Here I present evidence in favor of this assertion and claim that this is, in effect, a falsification of CDM on the scale of galaxies.

#### 1. Introduction

It is evident that a significant number of physicists are willing to devote their careers to the direct detection of dark matter particles. This intense investment of time, energy, and money reflects the perceived importance of this problem and its relevance to fundamental physics. What is the identity and nature of 80% of the mass content of the Universe and what does this tell us of physics beyond the Standard Model? Yet, in spite of the monumental and creative efforts, there is no convincing evidence that dark matter particles have been detected (leaving aside the controversial DAMA result). At present, dark matter is only evidenced by its putative global gravitational effect in large astronomical systems; as long as this is true, its presumed existence is not independent of the assumed form of the law of gravity or inertia on astronomical scales. In view of this, consideration of alternatives (e.g., a theory of gravity enlarged beyond General Relativity) would not unreasonable.

The only observationally viable alternative is modified Newtonian dynamics (MONDs), an ad hoc modification of Newton’s law of gravity or inertia proposed by Milgrom [1] more than 25 years ago. The phenomenological foundations for MOND come down to two observational facts about spiral galaxies. (1) The rotation curves of spiral galaxies are asymptotically flat, and (2) there is a well-defined relationship between the rotation velocity in spiral galaxies and the luminosity—the Tully-Fisher (TF) law [2]. This latter implies a mass-velocity relationship of the form where is in the neighborhood of 4.

The phenomenon of flat rotation curves is well known, and an example is shown in Figure 1. The rotation curve, measured in the 21 cm line of neutral hydrogen, extends well beyond the visible disk of the galaxy and shows no indication of a decline, certainly not a Keplerian decline.

One can conceive of several modifications which could yield flat rotation curves. But Milgrom realized that the only modification leading to a Tully-Fisher law with a logarithmic slope of four is one in which a deviation from Newton’s law appears not at large distance but at low acceleration. His suggestion, viewed as a modification of gravity, was that the actual gravitational acceleration is related to the Newtonian gravitational acceleration as

where is a new physical parameter with units of acceleration and is a function which is unspecified but must have the asymptotic form when and where .

The immediate consequence of this is that, in the limit of low accelerations, . For a point mass , if we set g equal to the centripetal acceleration , this gives

in the low acceleration regime. So all rotation curves are asymptotically flat and there is a mass-luminosity relation of the form . These are aspects that are built into MOND so they cannot rightly be called predictions. However, in the context of MOND, the aspect of an asymptotically flat rotation curve is absolute. MOND leaves rather little room for maneuver; the idea is in principle falsifiable, or at least it is far more fragile than the dark matter hypothesis. Unambiguous examples of rotation curves (of isolated galaxies) which decline in a Keplerian fashion at a large distance from the visible object would falsify the idea.

In addition, this mass-rotation velocity relation (2) forms the basis of the observed Tully-Fisher relationship, a luminosity-rotation velocity correlation of the form . In so far as the mass-to-light ratio in spirals is roughly constant, the TF relation should be the same for different classes of galaxies and the logarithmic slope must be four. Moreover, the relation is essentially one between the total baryonic mass of a galaxy and the asymptotic flat rotational velocity—not the peak rotation velocity but the velocity at large distance. This is the most immediate and most obvious prediction [3, 4].

The near-infrared TF relation for the Ursa Major sample of spiral galaxies [5] is shown as a log-log plot in Figure 2, where the velocity is that of the flat part of the rotation curve. The scatter about the least-square fit line of slope is consistent with observational uncertainties (i.e., no intrinsic scatter). Given the mean near-infrared mass-to-light ratio of about one, this observed TF relation (2) tells us that must be on the order of cm/s^{2}. It was immediately noticed by Milgrom that to within a factor of 5 or 6. This cosmic coincidence suggests that MOND, if it is right, may reflect the effect of cosmology on local particle dynamics.

#### 2. General Predictions

There are several other immediate consequences of modified dynamics which were previewed by Milgrom in his original papers.

The critical acceleration may be rewritten as a surface density

If a system, such as a spiral galaxy, has a surface density of matter greater than , that means that the internal accelerations are greater than , so the system is in the Newtonian regime. In systems with (high surface brightness or HSB galaxies) there should be a small discrepancy between the visible and classical Newtonian dynamical masses within the optical disk. But in low surface brightness (LSB) galaxies () there is a low internal acceleration, so the discrepancy between the visible and dynamical masses would be large. By this argument Milgrom predicted, before the actual discovery of a large population of LSB galaxies, that there should be a serious discrepancy between the observable and dynamical masses within the luminous disk of such systems—they should exist. They do exist, and this prediction has been verified [3].

Rotationally supported Newtonian systems tend to be unstable to global nonaxisymmetric modes which lead to bar formation and rapid heating of the system [6]. In the context of MOND, these systems would be those with , so this would suggest that should appear as an upper limit on the surface density of rotationally supported systems. This critical surface density is 0.2 g/cm^{2} or 860 /pc^{2}. A more appropriate value of the mean surface density within an effective radius would be or 140 /pc^{2}. Taking , this would correspond to a surface brightness of about 22 mag/arc sec^{2}. There is such an observed upper limit on the mean surface brightness of spiral galaxies and this is known as Freeman’s law [7, 8]. The existence of such a limit becomes understandable in the context of MOND.

Spiral galaxies with a mean surface density near this limit—HSB galaxies—would be, within the optical disk, in the Newtonian regime. So one would expect that the rotation curve would decline beyond the visible disk in a near Keplerian fashion to the asymptotic constant value. In LSB galaxies, with mean surface density below , the prediction is that rotation curves would rise to the final asymptotic flat value. So there should be a general difference in rotation curve shapes between LSB and HSB galaxies. In Figure 3, I show the observed rotation curves (points) of two galaxies, an LSB [9] and HSB [10], where we see exactly this trend. This general effect in observed rotation curves was first pointed out by Casertano and van Gorkom [11].

With Newtonian dynamics, pressure-supported systems which are nearly isothermal have infinite extent. But in the context of MOND it is straightforward to demonstrate that such isothermal systems are finite with the density at large radii falling roughly like [13]. The equation of hydrostatic equilibrium for an isotropic isothermal system reads

where in the limit of low accelerations . Here is the radial velocity dispersion and is the mass density. It then follows immediately that, in this MOND limit,

Thus there exists a mass-velocity dispersion relation of the form

that is similar to the observed Faber-Jackson relation (luminosity-velocity dispersion relation) for elliptical galaxies [14]. This means that a MOND near-isothermal sphere with a velocity dispersion on the order of 100 km/s will always have a galactic mass. It also means that a near-isothermal object with a velocity dispersion of 1000 km/s will have the mass of a cluster of galaxies, and an object with a velocity dispersion of 5 km/s will have the mass of a globular star cluster. In other words, the same Faber-Jackson law should apply to all pressure supported near-isothermal objects. For Newtonian systems, the existence of such a relationship must be explained by the contingencies of structure formation rather than existent dynamics. Because of the appearance of an additional dimensional constant, , in the structure equation (5), MOND systems are much more constrained than their Newtonian counterparts.

But with respect to actual pressure supported systems, an even stronger statement can be made. Any isolated system that is nearly isothermal will be a MOND object. That is because a Newtonian isothermal system (with large internal accelerations) is an object of infinite size and will always extend to the region of low accelerations (). At that point (), MOND intervenes and the system will be truncated. This means that the internal acceleration of any isolated isothermal system () is expected to be on the order of or less than and that the mean surface density within will typically be or less (there are low-density solutions for MOND isothermal spheres, , with internal accelerations less than ).

Figure 4 shows the observations [15]. This is log-log plot of velocity dispersion versus size for systems spanning many orders of magnitude from subgalactic to supergalactic systems (the identity of the systems is noted in the caption). The straight line is not a fit but rather the locus of . We see that the internal acceleration of these systems all lie with in a factor of a few of . It is not evident how dark matter would explain this, but such a fact would certainly seem to be a challenge that should not be ignored.

#### 3. Rotation Curve Analysis

The most impressive phenomenological success of MOND is in predicting the form of galaxy rotation curves from the observed distribution of detectable matter—stars and gas [3, 5, 12]. The procedure followed is described in detail by Sanders and McGaugh [15]. Basically, one assumes that light traces mass, that is, the mass-to-light ratio (*M*/*L*) in any individual galaxy is constant. Then, after converting the surface brightness distribution (preferably in the near infrared) into a surface density distribution and including the contribution of the gas which is observed directly, the Newtonian gravitational force, , is calculated via the classical Poisson equation. Here it is usually assumed that the stellar and gaseous disks are razor thin. The “true” gravitational force, , is calculated from the MOND formula with fixed, and the mass of the stellar disk is adjusted until the best match to the observed rotation curve is achieved. This gives *M*/*L* of the disk as the single free parameter of the fit (unless a bulge is present).

In comparison to the observed rotation curve one assumes that the motion of the gas is coplaner rotation about the center of the given galaxy. This is certainly not always the case because there are well-known distortions to the velocity field in spiral galaxies caused by bars and warping of the gas layer. In a fully 2-dimensional velocity field these distortions can often be modeled, but the optimal rotation curves are those in which there is no evidence for the presence of significant deviations from coplaner circular motion. But it should be remembered that a perfect theory will not fit all rotation curves because of these possible problems (the same is true of a specified dark matter halo). The point is that with MOND, usually, there is one free parameter per galaxy and that is the mass or *M/L* of the stellar disk; with dark halos there are typically three free parameters: *M/L* of the disk, a length scale, and velocity dispersion (or total mass) for the halo.

Figure 3 shows two examples of MOND fits to rotation curves. The dotted and dashed curves are the Newtonian rotation curves of the stellar and gaseous disks, respectively, and the solid curve is the MOND rotation curve with cm/s^{2}. We see that, not only does MOND predict the general trend for LSB and HSB galaxies, but it also predicts the observed rotation curves * in detail* from the observed distribution of matter. This procedure has been carried out for about 100 rotation curves (see [15] for a more complete compilation of MOND rotation curves). In only about 10 cases the predicted rotation curve is significantly different from the observed curve, and for these objects there is usually an obvious problem with the observed curve or its use as a tracer of the radial force distribution. Moreover, there is the general impression that as the observational data improves, so does the agreement between the MOND and observed rotation curves (see, e.g., the higher resolution rotation curve of NGC 2903 from the THINGS survey [16]).

I have noted that the only free parameter in these fits is the mass-to-light ratio of the visible disk, so one may well ask if the inferred values are reasonable. Here it is useful to consider again the UMa sample [5] because all galaxies are at the same distance and there is K’-band (near infrared) surface photometry for the entire sample. The sample also contains both HSB and LSB galaxies. Figure 5 shows the *M/L* in the B-band required by the MOND fits plotted against B-V color (a) and the same for the K’-band (b). We see that in the K’-band with a 30% scatter. In other words, if one were to assume a K’-band *M*/*L* of one at the outset, most rotation curves would be quite accurately predicted from the observed light and gas distribution with no free parameters. In the B-band, on the other hand, the MOND *M*/*L* does appear to be a function of color in the sense that redder objects have larger *M*/*L* values. This is exactly what is expected from population synthesis models as is shown by the solid lines in both panels [17]. This is striking because there is nothing built into MOND which would require that redder galaxies should have a higher ; this simply follows from the rotation curve fits.

I have already shown three examples of observed rotation curves compared to the curve calculated with the MOND formula using the observed distribution of detectable baryons (Figures 1 and 3). I show one more in Figure 6 because it illustrates very well a point that I wish to emphasize. UGC 7524 is a dwarf low surface brightness galaxy [18]. In the Figure 6(a) I show the logarithm of the surface density in stars and gas as a function of radius (the stellar surface density is determined from the surface brightness distribution with MOND value of ). In Figure 6(b) I show again the observed rotation curve (points), the Newtonian rotation curves of stars and gas, and the MOND rotation curve. We see that, for both stars and gas, there is an enhancement in the surface density between 1.5 and 2.0 kpc, and of course, there is a corresponding feature in the Newtonian rotation curves. But we see that there is also a feature at this position in the total rotation curve, even though there is a significant discrepancy between the Newtonian and detectable mass. The total rotation curve perfectly reflects details in the observed mass distribution even though the object is “dominated by dark matter” in the inner regions.

This is an empirical point emphasized repeatedly by Sancisi [19]: * For every feature in the surface brightness distribution (or gas surface density distribution) there is a corresponding feature in the observed rotation curve (and vice versa)*. I would add that with dark matter this seems rather unnatural. How is it that the dark matter distribution can match so perfectly the baryonic matter distribution? But with MOND, it is expected. What you see is all there is!

It has been argued that such features in rotation curves could be due to streaming motions in the gas associated with spiral arms or other such deviations from circular symmetry. Perhaps so, but then this would clearly be project for detailed modeling. Can nonaxially symmetric distortions create in detail the observed fluctuations in rotation curves in the presence of a dominant halo? This should be seen as an additional challenge for the dark matter paradigm.

In general, the success of MOND in accounting for galaxy rotation curves with only one free parameter, the *M/L* of the visible disk which is usually found to have quite reasonable values, is striking. Whether the basic premise of MOND, that dynamics becomes nonNewtonian at low accelerations, is correct or not, the success of this simple algorithm implies that the detailed form of galaxy rotation curves is entirely determined by the distribution of visible matter. * If the mass discrepancy is due to dark matter then this phenomenology demands explanation*; it cannot be swept under the rug as being due to “messy astrophysics” or to unjustified claims that CDM halos possess an acceleration scale [20, 21]. This goes well beyond the issue of whether or not dark halos have cusps. The point is that rotation curves indicate the presence of a cusp if there is a cusp in the light distribution; if rotation curves imply no cusp, then there is no cusp in the light distribution.

#### 4. Clusters of Galaxies: A Phenomenological Problem for MOND?

It has been known for more than 70 years [22] that clusters of galaxies exhibit a significant discrepancy between the Newtonian dynamical mass and the observable mass, although the subsequent discovery of hot X-ray emitting gas goes some way in alleviating the original discrepancy. For an isothermal sphere of hot gas at temperature T, the Newtonian dynamical mass within radius , calculated from the equation of hydrostatic equilibrium, is

where is the mean atomic mass and the logarithmic density gradient is evaluated at . This dynamical mass turns out to be typically about a factor of five or six larger than the observed mass in hot gas and in the stellar content of the galaxies (see [23, Figure , left]).

With MOND, the dynamical mass (5) is given by

and, using the same value of determined from nearby galaxy rotation curves turns out to be, on average, a factor of two or three larger than the observed mass (Figure 7(b)). The discrepancy is reduced but still present. This could be interpreted as a failure [24], or one could say that MOND predicts that the mass budget of clusters is not yet complete and that there is more mass to be detected [23]. The cluster missing mass could, for example, be in neutrinos of mass 1.5 to 2 eV [25], or in “soft bosons” with a large de Broglie wavelength [26], or simply in heretofore undetected baryonic matter. It would have certainly been a falsification of MOND had the predicted mass turned out to be typically * less* than the observed mass in hot gas and stars.

#### 5. Cosmology and Structure Growth

MOND not only allows the form of rotation curves to be precisely predicted from the distribution of observable matter, but it also explains certain systematic aspects of the photometry and kinematics of galaxies and clusters. The presence of a preferred surface density in spiral galaxies and ellipticals—the so-called Freeman and Fish laws; the fact that pressure-supported nearly isothermal systems ranging from molecular clouds to clusters of galaxies are characterized by a specific internal acceleration (); the existence of a TF relation with small scatter—specifically a correlation between the baryonic mass and the asymptotically flat rotation velocity of the form ; the Faber-Jackson relation for ellipticals, and with more detailed modeling, the Fundamental Plane [27]; not only the magnitude of the discrepancy in clusters of galaxies but also the fact that mass-velocity dispersion relation which applies to elliptical galaxies (7) extends to clusters (the mass-temperature relation). And it accomplishes all of this with a single new parameter with units of acceleration—a parameter determined from galaxy rotation curves which is within an order of magnitude of the cosmologically significant value of . This is why several of us believe that, on an epistemological level, MOND is more successful than dark matter and, in fact, constitutes a falsification of dark matter on the scale of galaxies.

But, of course, MOND must fit into a larger picture. What are the larger-scale consequences of modified dynamics—specifically what are the implications for gravitational lensing and cosmology? Does MOND provide a mechanism for structure formation in a low density universe? These are questions which require a more basic theory underlying MOND, and there has been considerable progress in this respect as well.

I would first like to stress that MOND is not necessarily at odds with cherished physical principles. Soon after Milgrom’s original papers, Felten [28] pointed out that the conservation of linear and angular momentum for an N-body system is violated by Milgrom’s simple formula. This had already been appreciated by Bekenstein and Milgrom [29] who reformulated MOND as a Lagrangian-based, modified Poisson equation.

where is the (scalar) gravitational field and the function must have the asymptotic behavior required in the simple MOND prescription. In this form the usual conservation laws are respected. Moreover, this kind of nonlinear field equation appears in other contexts in physics; for example, it is identical to Maxwell’s first equation in a nonlinear isotropic medium where the dielectric parameter is a function of the electric field strength.

Going beyond this nonrelativistic formulation, there has been considerable progress in constructing relativistic theories of gravity which, in the regime of very low field gradients, reproduce the phenomenology of MOND [29–31]. This has culminated in the tensor-vector-scalar theory (TeVeS) of Bekenstein, which is fully covariant and free of the anomalies of earlier attempts (such as superluminal propagation) [32]. The theory is complicated; it requires three additional parameters and a free function (one not specified by any a priori considerations but set to reproduce the phenomenology), but it does demonstrate that a covariant version of MOND is possible.

Milgrom [33] has considered the alternative point of view, that MOND, at a nonrelativistic level, may be due to a modification of the free particle action (modified inertia) resulting, possibly, from the interaction of a particle with vacuum fields [34]. Here, should appear as an effective constant for galactic systems, but, in general, the acceleration threshold for modified dynamics would be dependent upon the particle trajectory. In this case, one would expect Milgrom’s original formula to be only an approximation to the truth for generalized particle motion.

Given there is not yet a generally accepted theoretical basis for MOND it might seem premature to consider cosmological implications. None the less, several general points can be made. First of all, it is clear that the experimental foundations of the standard Big Bang are so well established, that any underlying theory of MOND should not lead to a radically different cosmology, at least not in the early radiation-dominated Universe and certainly not at the epoch of nucleosynthesis. Then, to say that MOND is an alternative to dark matter does not imply that undetected or dark matter is nonexistent. In fact undetected baryonic matter must be present because in visible matter is substantially less than in baryons. Moreover, there are clear indications that at least some flavors of neutrinos have a nonvanishing mass [35], so there is a contribution of nonbaryonic dark matter to the total mass budget of the Universe—at least at a level comparable to the mean density of baryons in visible stars. But it would be contrary to the spirit of MOND if dark matter—baryonic or nonbaryonic—was a dominant constituent of galaxies; that is, MOND is inconsistent with the existence of cold dark matter (CDM) which clusters on small scales. So the question arises—how robust is the cosmological evidence for CDM at the level required for the now standard concordance model of the Universe (CDM): roughly 70% “dark” energy and 30% CDM?

Support for the concordance model rests primarily upon the observations of distant supernovae [36], the angular power spectrum of the small-scale temperature fluctuations in the cosmic microwave background [37], and the amplitude of density fluctuations in the galaxy distribution as a function of scale. It is certainly true that the concordance model is consistent with these observations; however, this interpretation depends upon the validity of General Relativity and thereby, the validity of the Friedmann equation in describing the expansion history of the Universe. But if MOND is correct, then classical four-dimensional General Relativity does not give a proper description of reality on a cosmic scale. Indeed the peculiar composition of the Universe embodied by the concordance model has led some to suggest that modifications of standard General Relativity, and therefore late-time modifications of the Friedmann equation, are preferable. Often these modifications are based upon the currently popular braneworld scenarios [38]. But, recently, more ad hoc modifications have also been considered [39]. * It is curious that such alternatives to dark energy are considered acceptable on aesthetic grounds, while a conceptually similar, but empirically justified, alternative to dark matter is not. *

Of course, if we live in a Universe of only baryons and low-mass neutrinos, then how does structure form? After all a primary motivation for nonbaryonic dark matter is the necessity of forming the observed structure in the Universe by the present epoch via gravitational growth of very small density fluctuations. As we all know, nonbaryonic dark matter helps because it offers the possibility that fluctuations can begin growing before the epoch of hydrogen recombination. The expectation is that MOND, by providing stronger effective gravity in the limit of low accelerations, might also help, but in the absence of a proper theory, this question cannot be rigorously addressed (see, however, [40, 41]). Moreover, it appears that TeVeS can lead to structure formation on a level comparable to that of CDM [42].

Ideally, an underlying theory of MOND would make predictions on a scale other than extragalactic, and this would provide the possibility of a more definitive test. One general expectation is the appearance of deviations from gravity in the outer solar system where the accelerations are becoming low. In this respect, the recently reported anomalous constant acceleration apparently detected beyond the orbit of Jupiter by the Pioneer spacecrafts [43] is most relevant. If confirmed, this would certainly indicate a breakdown of Newtonian dynamics in the low acceleration regime.

#### Acknowledgment

The author is very grateful to Moti Milgrom, Jacob Bekenstein, and Stacy McGaugh for useful discussions.

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