In the sequel, eight predictions that follow from the hypothesis and support for them will be presented.
5.1. First Prediction
The first prediction is that the linear gravity coming from the superposed universe is still a valid solution of Einstein’s field equations, with some well explained natural source of the added logarithmic potential caused by dark matter, as proposed in chapter 4. The hypothesis in hand must give a natural explanation for this added gravitational potential and in the specific case of galaxy rotation, i.e., in the non-relativistic limit of GR, lead to the well-established Tully-Fisher relation
. In this section it will be shown that the cylindrically symmetric solution of Levi-Civita [
5] as worked out by Santos et al. [
6] is a working solution for galaxies and flat rotation curves and it will be shown it is indeed consistent with the linear gravity hypothesis.
The Schwarzschild metric is a solution of Einstein’s field equations for an empty space with only a point-mass
M, like the galactic centre. The Schwarzschild line element is as follows:
Which in the Newtonian approximation becomes
= 1 + 2
. This leads to the Newtonian potential that is proportional to 1/
R. But in 1919 Levi-Civita found the solution for a cylindrical vacuum spacetime, which has the following form:
Santos et al. show that in the Newtonian limit, this metric yields the logarithmic potential:
Here
r is the radial coordinate, i.e., the distance to the axis of the cylinder. The constant
a in (6) must have the value unity to be consistent with the Minkowski flat space when σ = 0 [
6] (p. 6). Besides this, it does not appear in the gravitational potential that results from (10), as can be seen up here, so it is put to unity in the sequel. Now, since the theory in hand does not in any way modify this description of gravity, but only states that the dark mass should be projected at larger distances, because of the stretching of the rolled up dimensions, this metric can still be used without modifications or added terms.
Modelling the total mass acting in a galaxy as a visible point mass together with a set of dark matter line-masses would yield the sum of both a linear and a logarithmic potential. Now, the hypothesis in hand for a wire-mass leads to
, in which
G is the gravitational and
M’ the linear mass density, i.e., mass over thickness of the galaxy disc, in line with Santos et al. [
6]. So, the line element to model dark matter in galaxies becomes:
This is utterly consistent with the conclusions of Santos et al., who conclude that
must be the Newtonian mass per unit length as produces by an infinitely long line-mass, which as well Levi-Civita himself already concluded [
6] (p. 4 and p. 11).
These two metrics (5) and (8) cannot be added straightforwardly in GR, since GR is strongly non-linear. However, in very weak fields, GR can be treated as linear, using linearized GR, see [
3] (p. 18) and [
26] (p. 200). This is derived by treating the metric as split in two components:
, i.e., the Minkowski flat space and an added small deviation, so with
. The same can be done with the line element, denoting the deviation as
h simply. Comparing Milgrom’s constant with, for example, Earths gravitational acceleration makes clear this is a valid approach in galaxies. And in chapter 5.3 it will be shown in the Newtonian limit it gives an improved prediction method for rotation velocities, compared with MOND and T
eV
eS. So, upon studying flat rotation curves, these metrics may be added to one another to yield a valid solution of GR. As a result, the Newtonian potential and the logarithmic one (12) that followed from (11) will add up. This combination of metrics yields a good way to model dark matter n GR in weak fields, without the need to modify GR. In stronger fields, the point-mass and line-mass can only be combined in a numerical manner.
Now,
M’ being the linear mass density, i.e., mass over thickness of the galaxy disc, directly leads to the Tully-Fisher relationship
, since, as further explained in chapter 5.2, the thickness
d of the galaxy disc controls this mass density. The larger
d for a certain galaxy mass, the lower the mass density. In the next section
d will be taken proportional to the vertical disk scale length
hz. It can be shown with dedicated literature, for example de Kregel et al. [
44] that this, together with the disk scale length
hr, is proportional to the flat rotation velocity squared, i.e.,
. See
Figure 4. The summarizing SPARC data-table Table1.mrt [
11,
12] clearly confirms this. So,
d can be written as
. Since the logarithmic potential leads to
, so with
d appearing in the denominator of the right-hand-side of formula (8) in chapter 4.4, the latter two proportionalities simply lead to the Tully-Fisher relationship
.
But, the above is about visible baryonic disks, while the dark matter is described by a wire-like mass, existing in superposed universes. However, as argued in chapter 4.2 there will be strong correlation between the mass and rotation velocity of the baryonic mass and the dark matter, since larger amounts of baryonic mass will capture larger amounts of dark matter. And, this simply is in line with the findings of conventional cosmology with this respect, as for example is illustrated by the existence of the spin-parameter by Mo et al. [
40] which relates the baryonic disk and halo radii tightly together. So, it can be assumed that the above applies as well to the length and hence the linear mass density of the wires.
Comparing this with the alternative formulation following from MOND,
, shows Milgrom’s constant has a deeper relationship with 1/
d and hence with the vertical disk scale length
hz. It takes the place of the average ratio of velocity and scale height, so
, which is indeed an acceleration scale. An increasing rotation velocity tends to increase
hz, but there must be a counteracting force too, which is the gravitational attraction of the mass in the disk towards the disk plane. This is easily seen when one considers the height
hz a ball reaches when thrown upwards in the Earth’s gravitational field. Kinetic versus potential energy determines the height the ball reaches. This height is proportional to the square of the velocity
V divided by the acceleration due to gravity
g, i.e.,.
, which yields,
, with
. Comparing this with the expression that followed from MOND, Milgrom’s constant takes the place of the
average Newtonian gravitational acceleration g towards the disk plane of a large set of galaxies. Since dark matter in the article in hand is baryonic mass in superposed universes, i.e., universes with an alternative history, it in the deepest sense is the average
g over a large set of ‘dark’ galaxies intersecting with ours. So, MOND’s way of describing the effect of dark matter has a link with the linear mass density of the ‘wires’ too, by controlling
d through the acceleration that is expressed by
am. However, since
GL appears in formula (8) in the article in hand it is not predicted that this acceleration appears as a constant in galaxies in our universe. These findings will be further applied in the next section, upon applying the SPARC data [
11,
12].
5.2. Second Prediction
The second prediction is that the additional acceleration can be modelled by a set of additional dark galaxies that appear stretched in one or more directions, at least in the in the Newtonian limit, and that it is constant within each galaxy. It will be proportional to the amount of dark matter in a galaxy, which will vary between different galaxies. This has been done for all 175 galaxies from the SPARC database measured with the Spitzer Space Telescope [
11,
12].
The core assumption, as mentioned, is that the distribution of dark matter closely resembles the that of the visible matter, since they attract each other through gravity. This assumption is consistent with the findings of Lelli and Mistele [
9] mentioned in the introduction. They inferred the gravitational potential around isolated galaxies from weak gravitational lensing with the said SPARC data. With these data, they showed circular velocity curves that remain flat for hundreds of kpc, greatly extending the classic result from 21 cm observations. Indeed, they state there is no clear hint of a decline out to 1 Mpc, well beyond the expected virial radii of dark matter halos. This means the common way to project dark matter halos around galaxies cannot be valid. The hypothesis in the paper in hand clearly does not have this problem.
To assess the validity of this constant for linear gravity, firstly for all 175 galaxies the contributions of the visible baryonic matter distribution to the gravitational acceleration and from the invisible gas have been recalculated from the brightness profiles and HI-gas concentrations as reported by Starkman et al. [
12]. This has been done in a numerical manner by dividing the discs and bulges in a series of small patches and by evaluating all mutual attractions through gravity. This has been expressed in the form of velocity contributions, as the SPARC team did too. For the visible disk contribution, it is called
Vdisk and for the HI gas
Vgas. This done in order to verify and show that the author has interpreted the brightness profiles from the visible disk, from the bulges and the gas mass distributions correctly.
Figure 5 shows the contributions to gravitational acceleration as a function of radius distance. It is plotted for the galaxies NGC 6503 and NGC 6674, the first of which with a bulge contribution, called
Vbulge. The ‘
recalc’ subscripts refer to the values as calculated by the author, The ‘
SPARC’ indications refer to the values as reported by Starkman [
12] at the website, in the file MaximumDisk_Mass_Models_mrt.txt. This is the file produced by [
12]. It contains disk brightness profiles as well as observed rotation velocities
, Vobs and bulge brightness profiles as well as the theoretical velocities as calculated by the SPARC team with Newton’s law of gravity. It also contains error estimates, except for
Vbulge and for the HI gas
Vgas. As a consequence, for those variables, no error bars will be shown in the graphs down here in
Figure 5 and in the Annexes.
The squared theoretical velocities can be added and then result in the total Newtonian or baryonic gravitational acceleration, which can as well be expressed as a velocity contribution
Vbar. But the contribution of
Vdisk and
Vbuls depend on the mass-light-ratio
Yml, as follows:
Vgas in particular can have a significant negative contribution from gas outside the observed radius. Therefore, it is multiplied with its absolute value here to maintain the correct sign.
The mass-light-ratio, Yml is assumed 1 at this stage and will later act as the single fitting parameter. The contributions are calculated from the brightness profiles under the assumption that in thin disks the latter directly represent a distribution of the mass density. In the bulges this is not true; here brightness represents a cumulative mass density distribution since all observations of brightness run through the entire bulge and each layer adds brightness to the inward layers. So, it must be converted to a distributive mass distribution first, by subsequently subtracting the brightness contributions from larger radii at each observed radius, the part between two radii considered as a slice of a sphere. A complication with this is that the integration path length through each slice of the bulge is dependent on the radius observed. For example, at the most inner radius the brightness contribution from the outmost slice is much smaller than at the second outmost radius, since there one looks a long way perpendicularly through the outmost slice.
The HI-gas densities have been retrieved from the reported total HI mass and from the reported HI-radius by fitting the reported
Vgas to the formula from Martinsson [
46], see formula (10). Three of the parameters that were fixed by Martinsson have been replaced by fitted parameters a, b and
The latter is fitted to match the total reported HI mass of the galaxy. Multivariate regression has been used to find the optimal values in:
Following Lelli [
11], the total gas mass has been multiplied by a factor of 1.33 to account for helium gas as well. Following Patra [
47] the vertical scale length of the HI-gas is modelled three times bigger than
hz, because this reference among others mentions values up to 1 kpc which is three times bigger than mean value of the SPARC data set. Both scale lengths have been modelled explicitly, which means that for both the disk and the bulge a 3-dimensional model has been used.
Since, as mentioned, the goal of the calculations in the above merely is to verify and show that the author has interpreted the brightness profiles from the visible disk, from the bulges and the gas mass distributions correctly and not to obtain an improved mass-model, for some galaxies interpolations and extrapolations of the brightness profiles have been made to come closer to the SPARC graphs.
Then gravitational acceleration for each particle at each radius and each angle of its orbit and each distance from the central line of the disk can be calculated by summing up masses in each part of the galaxy disk and bulge with:
G is Newtons constant of gravity. Mass outside the orbit of each particle as far as it is not at the side of the centre of rotation as seen from the particle has a negative sign since it has a negative contribution to the centrifugal force. X is the distance between two masses.
Gravitational acceleration as observed in each galaxy, is calculated from the observed velocities
Vobs i.e., from the centrifugal force. This
Vobs is plotted in
Figure 6, as well as the baryonic contribution to the acceleration expressed as
Vbar, see its definition in formula (9). The lines
Vmond and
Vrecalc will be discussed in chapter 5.3.
The mass-to-light ratio has been used as the only fitting parameter to fit the baryonic rotation velocity, and hence the baryonic gravitational acceleration in each galaxy to the observed values near the core of the galaxies. After that, the hypothesis in hand is used to predict the additional gravitational acceleration at all radii without any further fitting.
The Newtonian gravitational accelerations, expressed by
Vbar, are now calculated with a fitted mass-to-light ratio,
Yml. It has for each galaxy simply be fitted such that
Vbar < 0.9
Vobs, at all radii, so following the sub-maximal disk hypothesis, in line with the findings of Lelli [
11]. This value of the ratio of 0.9 gives the best overall predictive performance of MOND for the 175 galaxies, after testing a range of values and it gives the most flat rotation curves with the currently proposed scenario. This assumes that the contribution from the Newtonian gravity never can be larger than the observed value, with some margin at all radii, so assuming there always is some contribution of dark matter at the smallest radii where Newtonian gravity will dominate too.
The error bars have been computed from the error estimates provided by the SPARC team, which concern
eVdisk,
eVbar, eVobs and the error of the disk surface brightness
eSBdisk. It has been assumed that deviations occurring in the measurements of the surface brightness at each radius are independent from each other and that those measurements are independent from the measurements of the rotation velocities and from the calculated velocities. Furthermore, the contributions of
eSBdisk. at specific radii have been weighted with the inverse of the squared distance
of each mass
mi as defined in formula (11) to the observed point.
. The errors in the variables computed in formula (11) have then be combined at each radius
R after Ku [
48] (pp. 265-269).
Now, for the scenario as predicted by the theory in hand, the gravitational contributions from dark matter, i.e., space in other universes appearing stretched to us, has been modelled in exactly the same manner, but using a loop over all 165 possible scenarios as summed up in
Table 1. Gravitational acceleration at the central line through the plane of rotation has been recalculated over the full three dimensions of the disk, the bulge and the gas cloud, comparable with the procedure in formula (11), so over all other particles
i at radii within the observed radius and outside, for all azimuths. This has been done in a exactly the same numerical manner, so with a limited resolution of patches at different radial distances and for 24 azimuth angles and assuming a vertical scale length
hz as calculated from the disk scale length ratio
hr/
hz, defined after Kruijt [
49] (p. 11) and Sparke and Gallagher [
50] (p. 202). The latter reference states at that page that typically the disk is about 10% as thick as it is wide, so
hr/
hz ≈ 10. As said, based upon [
47] for the gas the common factor three to increase
hz has been used. This yields a vertical mass distribution that then has been stretched in one or more directions according to
Table 1.
It should, however, be noted that in the disk and gas cloud a certain amount of ‘viscosity’ because of magnetism occurs, see Begelman & Rees [
42] (pp. 66 and 67), This yields an exchange of angular momentum over the disks cross dimension. As a result, still one value of
Vbar and
Vobs can still be attributed to or measured at each radius in the galaxy.
Then for each galaxy, the ratio of the dark matter in each superposed galaxy to the baryonic matter in our universe is denoted MLratio. This value could be optimised in a loop to give the best match between the observed and predicted flat parts of the rotation curves, which is deemed allowable since the theory does not predict the baryonic and dark masses should be the same. The amount of matter in the galaxies in the superposed universes can vary according to their history, since there is no fundamental reason why it should be exactly distributed as in our universe. The same, however, applies to the vertical scale length hz, of the dark galaxies compared to the galaxies in our universe. The mass ratio and the ratios of hz together determine the linear mass density in the dark galaxies, which is the true factor that determines the gravitational acceleration caused by a wire-mass. Therefore both could be optimised. To avoid huge numerical effort the choice has been made to optimise the hz proportional to this ratio in all cases, by modifying the stretch factor F, since some preliminary tests showed this gives the best rotation curve fits.
The values of
MLratio for the case the dark and visible galaxies are outlined with the coordinate axes as depicted in
Figure 3 have been plotted in
Figure 7. The average over
all tilting angles relative to the axes, which can be randomly divided, taken over all 175 galaxies and all angles should equal unity. They show a certain bandwidth, which indicates that the amount of dark matter or the vertical scale height can vary between different galaxies and have a different proportion to the visible matter. After all, the values of
MLratio represent the effect of the matter in the superposed universes as observed in our galaxies. Therefore a range of tilting angles and a range of observation points in the rotation planes have been simulated, for all 175 galaxies. The are shown in
Table 2.
When runs 1, 2 and 4 are taken twice, for reasons of symmetry and so as to give all the four scenario’s the same weight, the average value indeed equals unity.
Then it is interesting to know how much each of the scenarios of
Table 1 contribute to the additional gravitational acceleration in galaxies. This has been worked out in
Table 3.
This shows that the dark universes with one stretched dimension are dominating in this scenario, which confirms the earlier statement that dark matter in first approximation can be modelled as a wire mass.
5.3. Third Prediction
The third prediction is that with this natural explanation and the formula’s (10) to (12) a prediction model for the total acceleration, glinear + gbar (as defined in formula (9)) can be made that is as accurate or even more accurate than MOND and TeVeS.
And, in galaxies (like in clusters), the predictive power of the present scenario is indeed greater, as will be shown in the sequel.
The proof of this prediction comes from the same 175 measurements with SPARC. To this end, The observed Newtonian gravitational accelerations, corrected with MOND or TeVeS using formula (4) are divided by the observed gravitational acceleration Vobs2/R. The values for the inclination of the 175 galaxies and the distances to ourselves have been taken from the SPARC database without varying them.
This differs from the approach of Lelli [
11] which varied these two parameters within the reported error margins, so as to find the best correspondence of MOND with the observations, based upon the assumption that
am is a constant. The future will show whether with smaller error margins in these parameters that will still hold. Since as mentioned in chapters 4 and 5.1 in the theory in hand
GL can vary, this approach is obsolete here.
So, in the article in hand, the inclination and distance are not varied, but just the reported values have been used, just to compare the predictions as they are with
Vobs. Optimisation of
GL has been done such that the r.m.s. error value of the deviations of
glinear + gbar from g
obs over all radii is minimised. Following Ku [
47] (p. 269) the error estimate has been calculated as the r.m.s. value of the 175 error estimates of
GL over
(175 the number of SPARC galaxies). This gives an error estimate of ± 0.02 [m
3 kg
−1 s
−2].
Both the predictions following from MOND and the
µ(y) variant used by Bekenstein [
3] have been plotted as function of the distance
Dist of the galaxy to ourselves in
Figure 10. This can be done, since in galaxies, because of the low velocities and the weak field, the non-relativistic limit of T
eV
eS is applicable and that is equivalent to MOND, only with a different function
µ(y) [
3].
As well the ratio of values predicted with the linear model presented in this paper and the observed accelerations, (glinear + gbar) / gobs have been compared for all 175 galaxies. The predictions lie closer to the observed values than MOND and TeVeS, when the square root of the deviations of gMOND and (glinear + gbar) compared to gobs are added for all radii of all 175 galaxies. To get here, the function µ(y) from TeVeS had to be solved in an iterative manner at each radius.
This was based upon fitting the mass-to-light ratio
Yml based upon the maximal disk hypothesis. This approach is used in the 175 plots in Annex 2 and in
Figure 10. The overall performance of MOND is slightly better than that of T
eV
eS. With dedicated values for the baryonic to dark mass ratio per galaxy, so consistent with the theory as outlined in chapter 4, used in the entire range of radii in a galaxy, the improvement is 27 to 34% as shown in
Table 4.
This is based upon the velocities Vgas and Vdisk as calculated by the SPARC team from the detailed density distributions they measured, resulting in Vbar.
After that, the Newtonian gravitational accelerations as calculated by that team were modified with MOND as well as Bekenstein’s TeVeS.
In Annex 2 all the 175 rotation curves with the predictions are depicted. Some show that the predictions with linear gravity,
Vlin, reproduce little more details of the observed rotation curves too, see for example
Figure 6 in the previous section and
Figure 8 down here for two additional ones. In the legends, T
eV
eS is indicated as
Vbekst in
Figure 8.
They have been made for the situation that the dark and visible galaxies are outlined with the axis system as described in
Figure 3. This appears to give the best match for galaxies with clearly flat rotation curves, which, by the way, might give a clue to why some rotation curves are more flat than others in the first place.
The error-bars in the graphs have again been calculated from the error margins as reported by the SPARC team with the assumption that the different quantities are independent.
But, what causes the improvements? The central point is that MOND and TeVeS do modify the gravitational acceleration
g acting on a mass. It can easily be seen that when the mutual interaction of a small and a large mass is considered, this violates the conservation of momentum, Bekenstein [
3]. The present predictions avoid this, by calculating the mutual acceleration for all separate masses, with linear dependence from the mutual distance. And as a result, the interpolation function of MOND and TeVeS, see formula (2) in chapter 2, has become obsolete now, since all mutual interactions of mases in a galaxy are treated separately and in a consistent manner, with conservation of momentum. And this has a large effect, because, given the MOND parameter
µ is order of 0.1 to 0.5 in the flat rotation part of the 175 SPARC galaxies (so
x in formula (2) adopt values in the range of 0,1 to 0,6). So, in the intermediate MOND regime This makes clear this MOND interpolation function is dominating the MOND predictions. Almost all the SPARC observation points are in this intermediate, and hence not in the deep MOND regime. As a result, the interpolation function, acting on
g on a mass is determining.
The question is what this brings in terms of improving calculation methods for galaxies or simulation models for the evolution of galaxies. The application of this present calculation scheme, alternative to MOND, would take the following steps for a given radius R in a galaxy:
Calculate the Newtonian gravitational acceleration at R, from the baryonic mass distribution with formulas (10) and (11).
From the same baryonic mass distribution, already available from step 1), calculate the additional linear gravitational acceleration by stretching the distance the gravitational force acts by the said factor of approximately 22 to 23, in one, two or three directions conforming to all 164 scenarios summed up in
Table 1.
Add the Newtonian gravitational acceleration to the 164 linear gravitational accelerations and compute the rotation velocity at R.
As said, the theory in hand states the dimensions of all the other universes are stretched, according to the scenarios in
Table 1. As well, the baryonic and dark galaxies attract each other and are assumed to have the same orientations because of gravity, but together they can be tilted in any direction with respect to the stretches dimensions, i.e., with respect to the axes. When a wide range of possible orientations (i.e., a range of 0 to 45° to the nearest axis) and a range of points in the 175 galaxies are simulated a mean value of the amount of stretching can be determined. The mean factor amounts to
F = = 23 ± 0.1, so the predicted GUT-scale to 23/2π = 3.5
x Lp. This approach works at all radii, without the need for a distinction between two regimes, and without an interpolation scheme between the two regimes, as with MOND. Simulations of clusters, discussed in the next section will decrease the predicted value of
F somewhat, and show an overall value of 22 was suggested up here under point 2.
5.4. Fourth Prediction
The fourth prediction is the theory in hand is able to significantly improve the predictions of the velocity dispersions in galaxy clusters compared with MOND and gives a valid explanation for the way dark matter acts in clusters.
The clusters show velocity dispersions that depend on the gravitational potential and obey the Virial theorem Milgrom [
52]. Milgrom used data from NGC clusters only, but Tian, McGaugh et al. [
53] analyzed the much larger Abell clusters as well. The data of both sources have been combined in the graph depicted in the sequel in
Figure 10.
The paper in hand proposes an approach, in which the real existence of dark matter of which the gravitational attraction acts over one or more stretched dimensions, is the starting point.
Again, it is assumed the number of superpositions amounts to N = 165. For the conventional approach based upon Newtonian gravity, the assumed ratio of the sum of baryonic and dark matter to baryonic matter only amounts to N = 6. The later ratio has been used in the validation of the Monte Carlo simulations of clusters that will be presented in the sequel.
The Newtonian, and the MOND approach, as well as the scenario proposed in this paper will be elaborated and used to predict the dispersion velocities from the mass M and the diameter Rh of the clusters.
The Virial theorem states that if a spherical distribution of objects of equal mass is stable and self-gravitating (such as a galaxy cluster), the total gravitational potential energy,
(U, of the objects is equal to minus two times the total kinetic energy,
T:
With
U being the sum of all the mutual gravitational potentials caused by the gravitational forces acting on test masses and the vectors to the mass centers, as follows:
For simple geometrical reasons it is commonly assumed the ratio between the squared velocity dispersion and the squared line-of-sight velocity, the latter being the actually measured quantity, amounts to 3. Then, equation (14) for Newtonian gravity typically results from dynamic N-body simulations or static Monte Carlo simulations for the line-of-sight velocity dispersions
σ2, after Navarro et al. [
54], Binney and Tremaine [
55], Lokas et al. [
56], Carlberg et al. [
57] Kravtsov et al. [
58] the Planck Collaboration [
59], Wolf et al. [
60], Evrard et al. [
61]:
In [
53] as well a factor 0.3 in this equation
(J = 3) is shown to give a close fit with the observations. With the radius
R200 = ½ Rh, the latter being the cluster diameter referred to in [
52] and [
53]. As shown in
Figure 11 this equation is in good correspondence with the said observational data, when as in conventional cosmology it is assumed the total amounts of matter amounts to approximately six times the baryonic matter. This factor
N = 6 has been applied to the data in the graph in
Figure 11 down here to yield the Newtonian velocity dispersions including the effect of dark matter.
But, Milgrom has applied the Virial theorem to the MOND formula (5) for spherical clusters in (Milgrom 2018). Milgrom’s formula for the dispersion velocity in a cluster is:
Contrary to Milgrom’s findings for smaller and nearer by clusters only, Milgrom [
52], the full range including the Abell clusters reveals the MOND data are significantly lower than the observations in the Abell clusters and the corresponding curve in
Figure 10 does not have the right slope.
Now, in line with the references cited in the above for this paper Monte Carlo simulations have been performed with Matlab
® to firstly reproduce formula (14) for reasons of validation. This has been done using an NFW-mass profile, see Navarro et al.l [
54] with a typical expected value for the concentration parameter of
c = 3 for large clusters and to 10 for smaller ones, after Bullock et al. [
62] and Groener et al. [
63], which then is varied statistically using a log-normal distribution around this value. This parameter
c is defined as
R200/r
s, see formula (16).
The reference density
is chosen so as to reproduce the total cluster mass
M200. In cosmological N-body or Monte Carlo simulations, the concentration parameter
c is log-normally distributed for a given mass, with a scatter in
log c of order 0.15–0.25, see Comerford & Natarajan [
64]. This supports the use of a log-normal Monte Carlo calculations with
σ ∼ 0.2–0.3 for variations in
c in NFW haloes e.g., Bullock et al. [
62]. Here
σ ∼ 0.2 has been applied using the ‘Randn’ function, to pull random figures from a standard normal distribution. The said value of
c is then taken as the mean expected value of the distribution (NGC 5005
c = 12, NGC, 5353:
c = 10, Abell 3526:
c = 6 and Abell 2142:
c = 3) and the value that has been pulled has the value e
(c +σRandn(N,1)), with
N the number of pulled values, which equals unity in each separate run.
The adopted distribution of the mass of individual galaxies is as well dependent on the radial position
r in a cluster, with larger galaxies prevailing near the cluster center. The corresponding radial dependence of the mass density is modelled as a saturated power law, motivated by dynamical friction and merger-driven mass segregation (e.g., Munari et al. [
65], De Lucia & Blaizot [
66]; Niederste-Ostholt [
67] van der Burg et al. [
68] Annunziatella M. et al. [
69] (showing Schechter functions describing the SMF that are much steeper in the outskirts than in the center; an effect that can be approximated with formula (17))). The adopted approximation is as follows, with
rref = 0.3 *
R200.:
This has been done up to the radius
R200 using the following galaxy masses:
Mfield = 3 *10
10 Msun and
Mcore = 4*10
10 Msun so as to match formula (14) and the observations exactly. Using the same Monte Carlo approach, the masses
M of each galaxy have varied analogue as the halo concentration parameter
c as described up here, following Bahé et al. [
70]. Based upon this reference a value of
σ ∼ 0.2 has been applied here as well. These values have been kept constant for the two largest clusters that have been simulated, Abell 3526 and Abell 2142, since the mass per galaxy does not vary significantly with cluster mass, see Lin et al. [
71] and decreased for the smallest two after [
71].
The velocity dispersions occurring in the simulation of each cluster have been determined for al 2400 galaxies and then the average value has been taken to make
Figure 10.
The radial resolution of the simulations varies from 20 radii for the smallest cluster to 250 for the largest one. The galaxies have been distributed over the radii so as to match with formula (16) and at each radius have been distributed equally over the corresponding spherical surface. The sensitivity of the results for this resolution has been verified and is negligible, since after the galaxies at a certain radius have been distributed over the surface of the sphere, a random rotation of in two directions has been applied to the galaxies at each radius in the cluster, to avoid biases caused by galaxies at different radii being placed too close to each other.
This has been simulated a dozen times for the said clusters, i.e., the largest in the said data set (Abell 2142) and three smaller ones (NGC 5005, NGC 5353 and Abell 3526) to validate the model with formula (14), before moving to a modified simulation conforming the theory in hand. The latter entails stretching the dimensions according to the 164 scenarios of
Table 1 in
Section 4.2, but furthermore with the same settings as the said validation simulation. This stretching, with say a factor
F, of one or more dimensions makes the gravitational force decrease faster, proportional to
F2. The amount of work a moving object has to perform is the integral of the force times the distance covered by a test mass, the distance covered being measured in our universe, so non-stretched. This simply means the gravitational potential contribution from another universe with a stretched dimension decreases with
F2 too. This means the isotropy of the velocity dispersions in a spherical cluster is broken when the contributions from other, stretched, universes are considered. For one stretched dimension, the integral, the mutual distance
expressed in terms of
x,y and
z- distances, and assuming movement in the x-direction is modified as follows:
The sum of this over all pairs of test masses is just equation (13). Upon stretching one dimension it will become:
The integral for movement in the
y (and likewise in the
z direction) however will become:
When two dimensions are stretched, for example both x and y, the potential for movement in the y-direction will as well be conforming to equation (18*) and when three dimensions are stretched all three will have this shape.
The gravitational potential varies with the radial distance from the galaxies to the centre of the cluster and at
R200 it converges to zero, see
Figure 9 for an example.
Upon employing formulas (18**), the assumed superposition of 165 universes with stretching of space in one, two or three directions as described
Table 1 has been modelled with the further unchanged Monte Carlo model. This exactly yields the same result as formula (14) and hence as the observations, provided for the factor
F a value of
F = 22 is adopted. The r.m.s. value of this factor
F over a dozen runs amounts to 3.4. Following Ku [
47] (p. 269) the error estimate has been calculated as this r.m.s. value over
(four the number of simulated clusters). This gives an error estimate of ± 1.7.
Figure 10.
Velocity dispersions in NGC and Abell clusters as function of cluster mass.
Figure 10.
Velocity dispersions in NGC and Abell clusters as function of cluster mass.
Formula (17) gives a reduction of the r.m.s. of the deviations from the observations of 44% compared with MOND and performs comparable with the conventional Newtonian approach.
The factor F = 22 ± 1.7 derived from these cluster velocity dispersions matches quite well with the factor derived from the 175 galaxies discussed in chapter 5.3, which amounted to F = 23 ± 0.1. To summarize, the description of dark matter as a result of 165 superposed universes in 11-dimensional space is fundamental to describe both flat rotation curves in galaxies and the cluster velocity dispersions in a consistent manner.
Then, like it was done with the galaxies, it is interesting to know how much each of the scenarios of
Table 1 contribute to the additional gravitational acceleration in galaxies. This has been worked out in
Table 5.
This distribution happens to be comparable to that in galaxies.