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**A Study of Dark Matter with Spiral Galaxy Rotation Curves. Part II** ()

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*International Journal of Astronomy and Astrophysics*,

**9**, 133-141. doi: 10.4236/ijaa.2019.92010.

1. Introduction

Dark matter in the core of spiral galaxies can exceed 10^{7} times the mean dark matter density of the Universe. For this reason we have studied spiral galaxy rotation curves measured by the THINGS collaboration [1] with the hope of constraining the properties of dark matter [2] . In “Part I” of this study [2] we integrate numerically the equations that describe the mixture of two self-gravitating non-relativistic ideal gases, “baryons” and “dark matter”. These equations require four boundary conditions: the densities
${\rho}_{h}\left({r}_{\mathrm{min}}\right)$ and
${\rho}_{b}\left({r}_{\mathrm{min}}\right)$ of dark matter and baryons at the first measured point
${r}_{\mathrm{min}}$ , and the “reduced” root-mean-square radial velocities
${\langle {v}_{\text{r}h}^{2}\rangle}^{\prime}{}^{1/2}$ and
${\langle {v}_{\text{r}b}^{2}\rangle}^{\prime}{}^{1/2}$ , defined as follows:

${\langle {v}_{\text{r}h}^{2}\rangle}^{\prime}\equiv \frac{\langle {v}_{\text{r}h}^{2}\rangle}{1-{\kappa}_{h}}\mathrm{,}$ (1)

and similarly for baryons. ${\langle {v}_{\text{r}h}^{2}\rangle}^{1/2}$ is the root-mean-square of the radial component of the dark matter particle velocities, and $0\le {\kappa}_{h}\le 1$ describes dark matter rotation, see [2] for details. In the present analysis we take ${\kappa}_{h}=0.15\pm 0.15\left(\text{syst}\right)$ [2] . The four boundary parameters are fit to minimize the ${\chi}^{2}$ between the rotation curves ${v}_{\text{obs}}\left(r\right)$ and ${v}_{b}\left(r\right)$ measured by the THINGS collaboration [1] , and the calculated rotation curves. The fits obtain rotation curves within the observational uncertainties. These fits are presented in Figures 1 to 10 of [2] , and the fitted parameters are presented in Table 1 of [2] .

In the present analysis we apply corrections and study all identified systematic uncertainties. We use the standard notation in cosmology as defined in [3] , and the values of the cosmological parameters therein. Occasionally we use units with $\hslash =1$ and $c=1$ as is customary.

2. Corrections from ${\rho}_{h}\left({r}_{min}\right)$ to ${\rho}_{h}\left(r\to 0\right)$

The first measured point ${r}_{\mathrm{min}}$ does not lie in the center of the spiral galaxy core, so we make a correction from ${\rho}_{h}\left({r}_{\mathrm{min}}\right)$ to ${\rho}_{h}\left(r\to 0\right)$ by numerical integration with the same equations and parameters described above. These corrections are presented in Table 1.

3. Measurement of the Adiabatic Invariant ${v}_{hrms}(\; 1\; )$

For each spiral galaxy we obtain the parameter

${v}_{h\text{rms}}{\left(1\right)}^{2}\equiv 3\langle {v}_{\text{r}h}^{2}\rangle {\left(\frac{{\Omega}_{c}{\rho}_{\text{crit}}}{{\rho}_{h}\left(0\right)}\right)}^{2/3}\equiv \frac{3k{T}_{h}\left(1\right)}{{m}_{h}}\mathrm{.}$ (2)

${v}_{h\text{rms}}\left(1\right)$ is the dark matter particles root-mean-square velocity extrapolated to the present time with expansion parameter $a=1$ in three dimensions, hence the factor 3. ${T}_{h}\left(1\right)$ is the temperature of dark matter of a homogeneous Universe at the present time. The parameter ${v}_{h\text{rms}}\left(1\right)$ is invariant with respect to adiabatic expansion of the dark matter. Note that for an ideal “noble” gas

Table 1. Corrections from ${\rho}_{h}\left({r}_{\mathrm{min}}\right)$ [2] to ${\rho}_{h}\left(r\to 0\right)$ . The statistical uncertainty is from the fit [2] . The systematic uncertainty is from the extrapolation from ${r}_{\mathrm{min}}$ to $r\to 0$ .

${T}_{h}{V}^{\gamma -1}=\text{constant}$ with $\gamma =5/3$ . By “noble” we mean that collisions (if any) between dark matter particles do not excite internal degrees of freedom (if any) of these particles. Alternatively, Equation (2) can be understood as ${v}_{h}\propto 1/a$ for non-relativistic particles in an expanding Universe. At expansion parameter $a$ when perturbations are still linear, and after dark matter becomes non-relativistic, the root-mean-square velocity of dark matter particles is

${v}_{h\text{rms}}\left(a\right)=\frac{{v}_{h\text{rms}}\left(1\right)}{a}\equiv {\left(\frac{3k{T}_{h}\left(a\right)}{{m}_{h}}\right)}^{1/2}\mathrm{.}$ (3)

Results are presented in Table 2. The average of ${v}_{h\text{rms}}\left(1\right)$ of 10 complete and independent measurements is

${v}_{h\text{rms}}\left(1\right)=1.192\pm 0.109\left(\text{tot}\right)\text{km}/\text{s}\mathrm{.}$ (4)

This result is noteworthy since the 10 galaxies used for these measurements have masses spanning three orders of magnitude, and angular momenta spanning five orders of magnitude [2] . Note that the correction in Table 1 has allowed us to include galaxy NGC 2841 in the average (this galaxy was excluded in [2] because the first measured point at ${r}_{\mathrm{min}}$ is at the edge of the galaxy core).

The expansion parameter ${a}_{h\text{NR}}$ at which dark matter becomes non-relativistic can be estimated from (3) as

Table 2. Presented are ${\langle {v}_{\text{r}h}^{2}\rangle}^{\prime}{}^{1/2}$ from Table 1 of [2] , and ${v}_{h\text{rms}}\left(1\right)$ defined in (2). ${\rho}_{h}\left(0\right)$ is taken from Table 1. ${\kappa}_{h}=0.15\pm 0.15\left(\text{syst}\right)$ [2] . The statistical uncertainties of ${\langle {v}_{\text{r}h}^{2}\rangle}^{\prime}{}^{1/2}$ and ${\rho}_{h}\left(0\right)$ are correlated [2] . The systematic uncertainty includes contributions from Table 1 and from ${\kappa}_{h}$ . The ${\chi}^{2}$ of these 10 measurements is ${\chi}^{2}=36.4$ , so the total uncertainty of the average has been multiplied by ${\left[36.4/\left(10-1\right)\right]}^{1/2}=2.0$ , as recommended in [3] .

${a}_{h\text{NR}}\approx \frac{{v}_{h\text{rms}}\left(1\right)}{c}\mathrm{.}$ (5)

There are threshold factors of O(1) presented in Section 5.

4. Dark Matter Mass ${m}_{h}$

We consider the scenario with dark matter dominated by a single type of particle (plus anti-particle) of mass ${m}_{h}$ . The mass density of a non-relativistic gas of fermions or bosons with chemical potential $\mu $ can be written as [4]

${\rho}_{h}={\langle {v}_{\text{r}h}^{2}\rangle}^{3/2}\frac{{N}_{f\mathrm{,}b}{m}_{h}^{4}}{{\left(2\text{\pi}\right)}^{3/2}{\hslash}^{3}}{\Sigma}_{f\mathrm{,}b}\mathrm{,}$ (6)

where the sums are

${\Sigma}_{f\mathrm{,}b}=\frac{{e}^{{\mu}^{\prime}}}{{1}^{3/2}}\mp \frac{{e}^{2{\mu}^{\prime}}}{{2}^{3/2}}+\frac{{e}^{3{\mu}^{\prime}}}{{3}^{3/2}}\mp \frac{{e}^{4{\mu}^{\prime}}}{{4}^{3/2}}+\cdots \mathrm{,}$ (7)

where ${\mu}^{\prime}\equiv \mu /\left(k{T}_{h}\right)$ , with upper signs for fermions, and lower signs for bosons. The sums for fermions and bosons are ${\Sigma}_{f}=0.76515$ and ${\Sigma}_{b}=2.612$ for chemical potential $\mu =0$ . ${N}_{f}$ ( ${N}_{b}$ ) is the number of fermion (boson) degrees of freedom. From (2) and (6) we obtain

${m}_{h}={\left[\frac{{\left(6\text{\pi}\right)}^{3/2}{\Omega}_{c}{\rho}_{\text{crit}}{\hslash}^{3}}{{v}_{h\text{rms}}{\left(1\right)}^{3}{N}_{f\mathrm{,}b}{\Sigma}_{f\mathrm{,}b}}\right]}^{1/4}\mathrm{.}$ (8)

Note that the measured ${m}_{h}$ is independent of ${\Omega}_{c}{\rho}_{\text{crit}}$ , see (2). From (4) and (8) we obtain

${m}_{h}=\left(53.5\pm 3.6\left(\text{tot}\right)\text{eV}\right)\cdot {\left(\frac{2}{{N}_{f}}\frac{0.76515}{{\Sigma}_{f}}\right)}^{1/4}\mathrm{,}$ (9)

for fermions, and

${m}_{h}=\left(46.8\pm 3.2\left(\text{tot}\right)\text{eV}\right)\cdot {\left(\frac{1}{{N}_{b}}\frac{2.612}{{\Sigma}_{b}}\right)}^{1/4}\mathrm{,}$ (10)

for bosons. Note that we have obtained these results directly from the fits to the spiral galaxy rotation curves, with no input from cosmology. The uncertainties in (9) and (10) include all statistical and systematic uncertainties listed in Table 1 and Table 2.

A non-relativistic non-degenerate ideal gas has

$\frac{\mu}{k{T}_{h}}=-\mathrm{ln}\left(\frac{\nu}{{\nu}_{Q}}\right),$ (11)

where $\nu \equiv V/N$ is the volume per particle, and ${\nu}_{Q}\equiv {\left[2\text{\pi}{\hslash}^{2}/\left({m}_{h}k{T}_{h}\right)\right]}^{3/2}$ is the “quantum volume”. For a non-degenerate ideal gas, $\nu /{\nu}_{Q}\gg 1$ so the chemical potential $\mu $ is negative, and increases logarithmically with particle concentration. Fermi-Dirac or Bose Einstein degeneracy sets in as $\mu \to 0$ . Note that in an adiabatic expansion $\mu /\left(k{T}_{h}\right)$ is constant.

Fitting spiral galaxy rotation curves, we obtain limits ${m}_{h}>16\text{\hspace{0.17em}}\text{eV}$ for fermions, and ${m}_{h}>45\text{\hspace{0.17em}}\text{eV}$ for bosons, at 99% confidence [2] . Equivalently, from (9) and (10), we obtain ${\Sigma}_{f}\lesssim 96$ for ${N}_{f}=2$ , and ${\Sigma}_{b}\lesssim 3.1$ for ${N}_{b}=1$ .

5. Transition from Ultra-Relativistic to Non-Relativistic Dark Matter

Consider dark matter in statistical equilibrium with chemical potential $\mu $ and temperature ${T}_{h}$ . This assumption is justified by the observed Boltzmann distribution of the dark matter [2] . We apply periodic boundary conditions in an expanding cube of volume ${a}^{3}V$ . The comoving number density of dark matter particles is [4] :

${n}_{h}{a}^{3}=\frac{{N}_{f,b}}{{\left(2\text{\pi}\hslash \right)}^{3}}{\displaystyle {\int}_{0}^{\infty}}4\text{\pi}{p}^{2}\text{d}p\frac{1}{\mathrm{exp}\left[\left(\sqrt{{m}_{h}^{2}{c}^{4}+{p}^{2}{c}^{2}/{a}^{2}}-{m}_{h}{c}^{2}-\mu \right)/\left(k{T}_{h}\right)\right]\pm 1}.$ (12)

The last factor is the average number of fermions (upper sign) or bosons (lower sign) in an orbital of momentum $p/a$ .

Now let dark matter decouple while ultra-relativistic, and assume no self-annihilation. Then ${n}_{h}{a}^{3}$ is conserved. In an adiabatic expansion, e.g. collisionless dark matter, the number of dark matter particles in an orbital is constant so $\mu $ and ${T}_{h}$ adjust accordingly. The problem has one degree of freedom, so we choose, without loss of generality, ${\mu}^{\prime}\equiv \mu /\left(k{T}_{h}\right)$ constant. ${T}_{h}\propto 1/a$ in the ultra-relativistic limit ( $k{T}_{h}\gg m{c}^{2}$ ), and ${T}_{h}\propto 1/{a}^{2}$ in the non-relativistic limit ( $k{T}_{h}\ll m{c}^{2}$ ). (In the transition between these two limits ${T}_{h}$ is momentum dependent.) Let us define $x\equiv pc/\left(ak{T}_{h}\right)$ , and ${y}^{2}\equiv {p}^{2}/\left(2{m}_{h}{a}^{2}k{T}_{h}\right)$ . In the ultra-relativistic limit

${n}_{h}{a}^{3}={A}_{f,b}{N}_{f,b}{\left(\frac{ka{T}_{h}}{\hslash c}\right)}^{3},\text{\hspace{1em}}{A}_{f,b}=\frac{1}{2{\text{\pi}}^{2}}{\displaystyle {\int}_{0}^{\infty}}\frac{{x}^{2}\text{d}x}{\mathrm{exp}\left[x-{\mu}^{\prime}\right]\pm 1}.$ (13)

In the non-relativistic limit

${n}_{h}{a}^{3}={\Sigma}_{f,b}{N}_{f,b}{\left(\frac{{m}_{h}k{a}^{2}{T}_{h}}{2\text{\pi}{\hslash}^{2}}\right)}^{3/2},\text{\hspace{1em}}{\Sigma}_{f,b}=\frac{4}{{\text{\pi}}^{1/2}}{\displaystyle {\int}_{0}^{\infty}}\frac{{y}^{2}\text{d}y}{\mathrm{exp}\left[{y}^{2}-{\mu}^{\prime}\right]\pm 1},$ (14)

as in (6). The intercept of these two asymptotes defines ${a}_{h\text{NR}}$ and ${T}_{h\text{NR}}\equiv {T}_{h}\left({a}_{h\text{NR}}\right)={T}_{h}\left(1\right)/{a}_{h\text{NR}}^{2}$ :

${m}_{h}{c}^{2}=2\text{\pi}{\left(\frac{{A}_{f,b}}{{\Sigma}_{f,b}}\right)}^{2/3}k{T}_{h\text{NR}},$ (15)

${a}_{h\text{NR}}={\left(\frac{2\text{\pi}}{3}\right)}^{1/2}{\left(\frac{{A}_{f,b}}{{\Sigma}_{f,b}}\right)}^{1/3}\frac{{v}_{h\text{rms}}\left(1\right)}{c}.$ (16)

For $\mu =0$ , we obtain for fermions ${A}_{f}=0.09135$ , ${\Sigma}_{f}=0.76515$ , ${m}_{h}{c}^{2}=1.523k{T}_{h\text{NR}}$ , and ${a}_{h\text{NR}}=0.7126{v}_{h\text{rms}}\left(1\right)/c$ ; and for bosons ${A}_{b}=0.1218$ , ${\Sigma}_{b}=2.612$ , ${m}_{h}{c}^{2}=0.8139k{T}_{h\text{NR}}$ , and ${a}_{h\text{NR}}=0.5209{v}_{h\text{rms}}\left(1\right)/c$ . Einstein condensation sets in at $\mu =0$ .

For $\mu /\left(k{T}_{h}\right)=-1.5$ we obtain for fermions ${A}_{f}=0.0220$ , ${\Sigma}_{f}=0.2074$ , ${m}_{h}{c}^{2}=1.409k{T}_{h\text{NR}}$ , and ${a}_{h\text{NR}}=0.6852{v}_{h\text{rms}}\left(1\right)/c$ ; and for bosons ${A}_{b}=0.02328$ , ${\Sigma}_{b}=0.2432$ , ${m}_{h}{c}^{2}=1.315k{T}_{h\text{NR}}$ , and ${a}_{h\text{NR}}=0.6620{v}_{h\text{rms}}\left(1\right)/c$ .

For $\mu /\left(k{T}_{h}\right)=-10.0$ we obtain for both fermions and bosons ${A}_{f,b}=4.6\times {10}^{-6}$ , ${\Sigma}_{f,b}=4.5\times {10}^{-5}$ , ${m}_{h}{c}^{2}=1.366k{T}_{h\text{NR}}$ , and ${a}_{h\text{NR}}=0.6747{v}_{h\text{rms}}\left(1\right)/c$ .

In summary, from the measured adiabatic invariant ${v}_{h\text{rms}}\left(1\right)$ we obtain ${m}_{h}$ and ${a}_{h\text{NR}}$ with (8) and (16) respectively. The ratio ${T}_{h}/T$ of dark matter-to-photon temperatures, after ${e}^{+}{e}^{-}$ annihilation while dark matter is still ultra-relativistic, is

$\frac{{T}_{h}}{T}=\frac{1}{\text{2\pi}}{\left(\frac{{\Sigma}_{f\mathrm{,}b}}{{A}_{f\mathrm{,}b}}\right)}^{2/3}\frac{{a}_{h\text{NR}}{m}_{h}{c}^{2}}{k{T}_{0}}\mathrm{,}$ (17)

where the photon temperature is $T={T}_{0}/a$ . Note that ${T}_{h}/T$ is proportional to ${v}_{h\text{rms}}{\left(1\right)}^{1/4}$ , and is proportional to $1/{T}_{0}$ . The intercept of the two asymptotes that we implemented allows direct comparison of (17) with ${T}_{h}/T$ in Table 7 of [2] .

6. Results for the Case $\mu =0$

We now specialize to the case of zero chemical potential $\mu =0$ corresponding, in particular, to equal numbers of dark matter particles and anti-particles, or to Majorana sterile neutrinos [5] , or to dark matter that was once in diffusive equilibrium with the Standard Model sector. We obtain from the measured adiabatic invariant ${v}_{h\text{rms}}\left(1\right)$ :

${m}_{h}=\left[53.5\pm 3.6\left(\text{tot}\right)\right]\cdot {\left(\frac{2}{{N}_{f}}\right)}^{1/4}\text{eV},$ (18)

${a}_{h\text{NR}}=\left[2.83\pm 0.26\left(\text{tot}\right)\right]\times {10}^{-6},$ (19)

$\frac{{T}_{h}}{T}=\left[0.423\pm 0.010\left(\text{tot}\right)\right]\cdot {\left(\frac{2}{{N}_{f}}\right)}^{1/4}$ (20)

for fermions, or

${m}_{h}=\left[46.8\pm 3.2\left(\text{tot}\right)\right]\cdot {\left(\frac{1}{{N}_{b}}\right)}^{1/4}\text{eV},$ (21)

${a}_{h\text{NR}}=\left[2.07\pm 0.19\left(\text{tot}\right)\right]\times {10}^{-6},$ (22)

$\frac{{T}_{h}}{T}=\left[0.507\pm 0.012\left(\text{tot}\right)\right]\cdot {\left(\frac{1}{{N}_{b}}\right)}^{1/4}$ (23)

for bosons. These uncertainties are valid for the considered scenario and include statistical uncertainties and all identified systematic uncertainties listed in Table 1 and Table 2. Systematic uncertainties unknown at present may be needed in the future.

These results can be compared with expectations in Table 7 of [2] (and its extensions for other ${N}_{f}$ and ${N}_{b}$ ). Note that ${T}_{h}/T$ is proportional to ${v}_{h\text{rms}}{\left(1\right)}^{1/4}$ , and proportional to $1/{T}_{0}$ , so it is highly significant that the measured ${v}_{h\text{rms}}\left(1\right)$ obtains ${T}_{h}/T\approx 0.4$ for $\mu =0$ . A different measured ${v}_{h\text{rms}}\left(1\right)$ , or a different ${T}_{0}$ , would have lead to the conclusion that $\mu \ne 0$ and/or dark matter was never in thermal equilibrium with the Standard Model sector. In conclusion, the measured value of ${v}_{h\text{rms}}\left(1\right)$ is strong evidence that $\mu =0$ and that dark matter was in thermal equilibrium with the Standard Model sector at some time in the early history of the Universe.

Measurements with individual spiral galaxies for the case of fermions with ${N}_{f}=2$ , e.g. sterile Majorana neutrinos, are presented in Table 3.

7. Additional Systematic Uncertainties?

Non-spherical spiral galaxies: Equations (3) to (6) of [2] are valid in general. So long as the numerical integration is along a radial direction in the plane of the galaxy, with $\nabla {P}_{h}={\stackrel{^}{e}}_{r}\text{d}{P}_{h}/\text{d}r$ and $\nabla \cdot {g}_{h}=\left(1/{r}^{2}\right)\text{d}\left({r}^{2}{g}_{h}\right)/\text{d}r$ , and similarly for baryons, there is no approximation, and no systematic uncertainty is needed.

Mixing of dark matter: So long as dark matter is assumed collisionless, the adiabatic invariant ${v}_{h\text{rms}}\left(1\right)$ should be exactly conserved, so we assign no systematic uncertainty to Equation (3).

New studies may require additional systematic uncertainties. However, at present we do not identify any.

Table 3. Measurements of the expansion parameter ${a}_{h\text{NR}}$ at which dark matter becomes non-relativistic, the dark matter particle mass ${m}_{h}$ , and the ratio of temperatures ${T}_{h}/T$ of dark matter-to-photons after ${e}^{+}{e}^{-}$ annihilation and before dark matter becomes non-relativistic. In this table the particles of dark matter are assumed to be fermions with ${N}_{f}=2$ and $\mu =0$ . The $1\sigma $ total uncertainties include the statistical and systematic uncertainties of ${v}_{h\text{rms}}\left(1\right)$ in Table 2. The ${\chi}^{2}$ 's are 36.4, 40.8, and 40.4 respectively, for 10 - 1 degrees of freedom, so the uncertainties of the averages have been multiplied by ${\left[{\chi}^{2}/\left(10-1\right)\right]}^{1/2}$ , as recommended in [3] .

8. Conclusions

A numerical integration obtains rotation curves for spiral galaxies [2] . This integration requires four parameters (boundary conditions). These parameters are obtained by a fit that minimizes the ${\chi}^{2}$ between the observed [1] and calculated rotation curves. The fits for ten spiral galaxies, as well as the fitted parameters, are presented in Reference [2] . The fits are in agreement with observations within observational uncertainties. Two of the measured parameters, that are of

interest to the present analysis, are ${\rho}_{h}\left({r}_{\mathrm{min}}\right)$ and ${\langle {v}_{\text{r}h}^{2}\rangle}^{\prime}{}^{1/2}$ , and are presented in

Table 1 and Table 2. From these two parameters we calculate the adiabatic invariant ${v}_{h\text{rms}}\left(1\right)$ defined in (2). Measurements of ${v}_{h\text{rms}}\left(1\right)$ for ten spiral galaxies are presented in Table 2. We obtain an average

${v}_{h\text{rms}}\left(1\right)=1.192\pm 0.109\left(\text{tot}\right)\text{km}/\text{s}\mathrm{.}$ (24)

This result is remarkable considering that the ten galaxies span three orders of magnitude in mass, and five orders of magnitude in angular momenta [2] .

We consider dark matter that is dominated by a single type of particle of mass ${m}_{h}$ . We assume that dark matter decoupled from the Standard Model sector and from self-annihilation while still ultra-relativistic. Then from ${v}_{h\text{rms}}\left(1\right)$ we obtain directly the expansion parameter at which dark matter becomes non-relativistic:

${a}_{h\text{NR}}\approx \frac{{v}_{h\text{rms}}\left(1\right)}{c}\mathrm{,}$ (25)

up to a threshold factor of O(1) presented in Section 5. From the adiabatic invariant ${v}_{h\text{rms}}\left(1\right)$ we also obtain the mass ${m}_{h}$ of dark matter particles, as a function of the chemical potential $\mu $ , with no input from cosmology, see (8).

The fits to spiral galaxy rotation curves allow us to set lower bounds to the dark matter particle mass ${m}_{h}$ [2] , and upper bounds to the dark matter chemical potential $\mu $ , that are not much greater than zero.

To proceed, we need to know the chemical potential $\mu $ of dark matter. We consider the scenario with $\mu =0$ which is appropriate for equal numbers of dark matter particles and anti-particles, or Majorana sterile neutrinos [5] , or dark matter that was once in diffusive equilibrium with the Standard Model sector. The upper bound to $\mu $ , obtained from the spiral galaxy rotation curves, is close to zero. A negative chemical potential would imply a dark matter temperature while ultra-relativistic higher than the temperature of the Standard Model sector, which seems implausible. In any case we proceed assuming $\mu =0$ , and obtain the results (18) to (23).

The ratio ${T}_{h}/T$ is proportional to ${v}_{h\text{rms}}{\left(1\right)}^{1/4}$ , and proportional to $1/{T}_{0}$ , so the result ${T}_{h}/T\approx 0.4$ is highly significant. A different measured adiabatic invariant ${v}_{h\text{rms}}\left(1\right)$ , or a different ${T}_{0}$ , could have obtained ${T}_{h}/T$ orders of magnitude different from unity, so the measurement ${T}_{h}/T\approx 0.4$ is strong evidence that dark matter was once in thermal equilibrium with the Standard Model sector, and gives added support to the scenario $\mu \approx 0$ .

We compare the measured ${T}_{h}/T$ and ${m}_{h}$ with expectations, see Table 7 of [2] (and extensions with other ${N}_{f}$ and ${N}_{b}$ ), and find one very good match: fermion dark matter with ${N}_{f}=2$ that decoupled in the approximate temperature range from the confinement-deconfinement transition to ${m}_{s}$ , that suggests Majorana sterile neutrino dark matter [2] ; and one marginal match for a boson with ${N}_{b}=3$ that decoupled in the temperature range from ${m}_{\pi}$ to ${m}_{c}$ .

Conflicts of Interest

The author declares no conflicts of interest regarding the publication of this paper.

[1] |
de Blok, W.J.G., et al. (2008) High-Resolution Rotation Curves and Galaxy Mass Models from THINGS. The Astronomical Journal, 136, 2648-2719. https://doi.org/10.1088/0004-6256/136/6/2648 |

[2] |
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[3] | Tanabashi, M., et al. (Particle Data Group) (2018) The Review of Particle Physics. Physical Review D, 98, Article ID: 030001. |

[4] | Hoeneisen, B. (1993) Thermal Physics. Mellen Research University Press, San Francisco. |

[5] |
Srivastava, Y.N., Widom, A. and Swain, J. (1997) Thermodynamic Equations of State for Dirac and Majorana Fermions. hep-ph/9709434. http://cds.cern.ch/record/334578/files/9709434.pdf |

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