1. Introduction
The dark matter density in the core of spiral galaxies can exceed 107 times the mean dark matter density of the Universe. To learn about the properties of dark matter, we study the rotation curves of spiral galaxies measured by the THINGS collaboration [1] . The galaxies studied are in a stationary state, i.e. they have pulled away from the expansion of the Universe.
We use the standard notation for cosmology as defined in [2] , and the values of the cosmological parameters presented therein. Sometimes we use units with
and
as is customary.
2. A Model of Spiral Galaxy Rotation Curves
Figure 1 presents rotation curves of the spiral galaxy NGC 3198 measured by the THINGS collaboration [1] . The observed rotation curve
has contributions from baryons
(stars in the disk and bulge, and gas), and from the halo of dark matter
:
(1)
These rotation velocities correspond, by definition, to test particles in circular orbits of radius r in the plane of the galaxy. There is good agreement between the THINGS analysis and previous measurements by K. Begeman [3] . The mass distribution of stars is obtained from measurements of surface brightness in the 3.6μm band and models of the mass-to-light ratio
. The mass distribution of gas is obtained from
maps. The uncertainties of
are from the THINGS observations and analysis [1] . We estimate the uncertainties of
from the scatter between 4 fits presented by the THINGS collaboration: “ISO, free”, “ISO, fixed”, “NFK, free”, and “NFK, fixed” [1] . These fits assume either the Navarro, Frenk and White (NFK) halo model [4] , or the pseudo-isothermal-gas (ISO) model.
From the measured rotation curves
and
we can obtain directly
and
. From
(assuming spherical symmetry) we can obtain
(2)
and similarly for
. We use these equations as cross-checks. Note that
Figure 1. Top figure: Observed rotation curve
(dots) and the baryon contribution
(triangles) of galaxy NGC 3198 obtained by the THINGS collaboration [1] . The “ISO, free” fit obtains
(dash-dotted line) [1] . The solid lines are obtained by numerical integration as explained in the text. The fitted parameters are given in Table 1. Bottom figure: Mass densities of baryons and of dark matter of galaxy NGC 3198 obtained by numerical integration as explained in the text.
and
are insensitive to whether or not the dark matter is rotating.
In the present analysis we would like to go further, i.e. constrain the equation of state of dark matter. To this end we compare the measured rotation curves with the following simplified model of a mixture of two self-gravitating non-relativistic ideal gases: “baryons” and “dark matter”. We assume that the interactions between baryons and dark matter can be neglected.
Table 1. Fitted parameters with
, and
. The last column shows the
of the fit and the number of degrees of freedom. The fits are presented in Figures 1-10.
(3)
(4)
(5)
(6)
and
are the mean-square of the velocity components in the radial direction
of baryons and dark matter respectively. Newton’s Equation (3) determine the gravitational field
due to the densities
of baryons and
of dark matter. Equations (5) express momentum conservation and are valid even for collisionless gases. The centrifugal acceleration terms proportional to
and
are inserted to study the rotation of baryons and dark matter.
We consider dark matter to be a mixture of interacting or non-interacting particles of masses
. Let
be the number density of dark matter particles of mass
with radial component of velocity between
and
. Then
(7)
where
(8)
and similarly for baryons. The pressure
is the momentum component in the radial direction in the galactic plane per unit time traversing unit area at r with
.
Equations (6) are the equations of state of the gasses. For the dark matter halo we have included a term due to the onset of degeneracy of fermions (upper signs) or bosons (lower signs).
(
) is the number of fermion (boson) degrees of freedom. We take
for one flavor of spin-up and spin-down sterile Majorana neutrinos. Results can be amended for other cases. For bosons we take
. Fermi-Dirac and Bose-Einstein degeneracy will be considered in Section 7. For now we set
to some large value, e.g.
eV, so the last term in Equation (6) is negligible.
We integrate numerically Equations (3) to (6) from
to
along a radial direction in the galactic plane. Hence
and
, and similarly for baryons.
Variables
and
, and also
and
, occur in the combinations
(9)
if the last term in (6) is negligible. To lift this degeneracy and obtain these variables separately, we need information in addition to the galaxy rotation curves.
We fit four parameters to minimize the
between the measured and calculated rotation velocities
and
: the starting densities
and
, and the “reduced” root-mean-square radial velocities
, and
. These parameters are boundary conditions at
and
. Assuming
and
are independent of r we obtain fits to the galaxy rotation curves that are in agreement with observations, within the experimental uncertainties, as shown in Figures 1-10, and in Table 1. The parameter correlation coefficients for galaxy NGC 3198 are shown in Table 2.
3. Derived Galaxy Parameters
We define
as the baryon mass contained within r, and similarly for
. Equations (3) to (6) allow the definition of several galaxy parameters: the “equal density radius”
with
, the “galaxy proper radius”
Table 2. Correlation coefficients of the four fitted parameters in Table 1 for galaxy NGC 3198.
at which
, and the corresponding “primordial comoving radius”
defined by
. The “baryon mass”
converges, so we define
. In the early Universe, when the perturbation that formed the galaxy was still linear, the matter of the galaxy was contained in the expanding sphere of proper radius
, and comoving radius
at
Figure 2. Top figure: Observed rotation curve
(dots) and the baryon contribution
(triangles) of galaxy NGC 2403 obtained by the THINGS collaboration [1] . The “NFW, free” fit obtains
(dash-dotted line) [1] . The solid lines are obtained by numerical integration for non-degenerate dark matter as explained in the text. The fitted parameters are given in Table 1. Bottom figure: Mass densities of baryons and of dark matter of galaxy NGC 2403 obtained by numerical integration as explained in the text.
Figure 3. Top figure: Observed rotation curve
(dots) and the baryon contribution
(triangles) of galaxy NGC 2841 obtained by the THINGS collaboration [1] . The “ISO, free” fit obtains
(dash-dotted line) [1] . The solid lines are obtained by numerical integration as explained in the text. The fitted parameters are given in Table 1. Bottom figure: Mass densities of baryons and of dark matter of galaxy NGC 2841 obtained by numerical integration as explained in the text.
time
. At time
the expansion parameter is
. The results, obtained with the four fitted parameters listed in Table 1, are presented in Table 3. The angular momenta of baryons
inside
are given in Table 4.
4. Estimate of
As an example, let us consider the spiral galaxy NGC 2403. A distribution of velocities along a particular line of sight is presented in figure 3 of [1] . The central value is ≈186 km/s, and the standard deviation is ≈11 km/s. So we estimate
. From Table 1,
km/s, and from Figure 2,
km/s. From these relations we obtain
, so the trajectories of stars and gas are approximately circular.
5. Estimate of
Consider an expanding sphere of proper radius
and comoving radius
at time
containing the matter that will become spiral galaxy NGC 2403. We assume adiabatic primordial perturbations, so the velocity fields of baryons and
Table 3. Galaxy parameters obtained by numerical integration with the fitted parameters in Table 1. See Section 3 for definitions.
Table 4. Baryon angular momentum
within radius
obtained by numerical integration (assuming
), and limits on
at 99% confidence.
is defined in Section 3.
of dark matter are the same. Then the angular momenta of baryons and dark matter in the sphere of proper radius
are in the ratio
. According to the model of hierarchical formation of galaxies [5] [6] , the sphere of radius
expands, reaches maximum expansion, and then collapses to form a galaxy, see figure 5 of Reference [6] . The angular momenta
and
are conserved if we neglect mixing. The density becomes approximately proportional
Figure 4. Top figure: Observed rotation curve
(dots) and the baryon contribution
(triangles) of galaxy NGC 2903 obtained by the THINGS collaboration [1] . The “ISO, free” fit obtains
(dash-dotted line) [1] . The solid lines are obtained by numerical integration as explained in the text. The fitted parameters are given in Table 1. Bottom figure: Mass densities of baryons and of dark matter of galaxy NGC 2903 obtained by numerical integration as explained in the text.
to
. If dark matter rotates with velocity
the angular momentum of dark matter of the galaxy of radius
is
. From the numerical integration for galaxy NGC 2403,
with
. Solving for
we obtain
.
For galaxy NGC 3198 we obtain
with
, and
.
Figure 5. Top figure: Observed rotation curve
(dots) and the baryon contribution
(triangles) of galaxy NGC 2976 obtained by the THINGS collaboration [1] . The “ISO, free” fit obtains
(dash-dotted line) [1] . The solid lines are obtained by numerical integration as explained in the text. The fitted parameters are given in Table 1. Bottom figure: Mass densities of baryons and of dark matter of galaxy NGC 2976 obtained by numerical integration as explained in the text.
6. The Boltzmann Distribution
Excellent fits to the rotation curves are obtained from Equations (3) to (6) with
and
independent of r, and non-degenerate dark matter. Since for the galaxies under consideration
and
, we will neglect the possible dependence of
and
on r. From (5) and (6) we obtain
Figure 6. Top figure: Observed rotation curve
(dots) and the baryon contribution
(triangles) of galaxy NGC 3521 obtained by the THINGS collaboration [1] . The “NFW, free” fit obtains
(dash-dotted line) [1] . The solid lines are obtained by numerical integration as explained in the text. The fitted parameters are given in Table 1. Bottom figure: Mass densities of baryons and of dark matter of galaxy NGC 3521 obtained by numerical integration as explained in the text.
(10)
where
is the gravitational potential. Note that
is conserved. So, within the observational uncertainties of the galaxy rotation curves, dark matter satisfies the Boltzmann distribution (10). This is a non-trivial
Figure 7. Top figure: Observed rotation curve
(dots) and the baryon contribution
(triangles) of galaxy NGC 3621 obtained by the THINGS collaboration [1] . The “ISO, free” fit obtains
(dash-dotted line) [1] . The solid lines are obtained by numerical integration as explained in the text. The fitted parameters are given in Table 1. Bottom figure: Mass densities of baryons and of dark matter of galaxy NGC 3621 obtained by numerical integration as explained in the text.
result. The derivation of the Boltzmann distribution in statistical mechanics assumes that the “system” under study is in “thermal equilibrium” with a “reservoir”,
and implies the equipartition theorem, e.g.
, which does not
hold between dark matter and baryons. There is no obvious “reservoir” interacting with the dark matter, so the well known derivation of the Boltzmann
Figure 8. Top figure: Observed rotation curve
(dots) and the baryon contribution
(triangles) of galaxy DDO 154 obtained by the THINGS collaboration [1] . The “NFW, free” fit obtains
(dash-dotted line) [1] . The solid lines are obtained by numerical integration for non-degenerate dark matter as explained in the text. The fitted parameters are given in Table 1. Bottom figure: Matter densities of baryons and of dark matter of galaxy DDO 154 obtained by numerical integration as explained in the text.
distribution may not apply to dark matter, unless dark matter was once in thermal equilibrium with “something”. Does the observed Boltzmann distribution suggest that dark matter was once in statistical equilibrium with the primordial (pre?) Standard Model cosmological soup?
7. Lower Bounds on mh for Fermions and Bosons
So far we have not considered the last term in Equation (6), i.e. we have set
Figure 9. Top figure: Observed rotation curve
(dots) and the baryon contribution
(triangles) of galaxy NGC 5055 obtained by the THINGS collaboration [1] . The “ISO, fixed” fit obtains
(dash-dotted line) [1] . The solid lines are obtained by numerical integration as explained in the text. The fitted parameters are given in Table 1. Bottom figure: Mass densities of baryons and of dark matter of galaxy NGC 5055 obtained by numerical integration as explained in the text.
to some high value. Note that we obtain excellent fits to the galaxy rotation curves assuming
with
independent of r. By lowering the value of
in the fits we can probe non-linearities between
and
. In particular, we study the onset of Fermi-Dirac or Bose-Einstein degeneracy of dark matter composed of particles of mass
. The dark matter density and pressure are [7]
(11)
Figure 10. Top figure: Observed rotation curve
(dots) and the baryon contribution
(triangles) of galaxy NGC 7793 obtained by the THINGS collaboration [1] . The “NFW, fixed” fit obtains
(dash-dotted line) [1] . The solid lines are obtained by numerical integration for non-degenerate dark matter as explained in the text. The fitted parameters are given in Table 1. Bottom figure: Mass densities of baryons and of dark matter of galaxy NGC 7793 obtained by numerical integration as explained in the text.
(12)
where
, and upper signs are for fermions, and lower signs are for bosons.
is the chemical potential. In the course of integrating Equations (3) to (6) numerically we need to obtain
given
and
. We do this by solving (12) for
and substituting the result in (11). We consider up to third order terms in the series of (11) and (12) until the onset of full degeneracy for fermions:
(13)
or the onset of Einstein condensation for bosons:
(14)
where the numerical factor is the ratio of the two series with
.
For bosons
. Einstein condensation sets in when
reaches 1. As
is lowered we find that
at
may exceed 1 indicating the onset of Einstein condensation. However the
of the fit to the galaxy rotation curves already exclude this value of
even when we increase the starting value of
within experimental bounds. In conclusion, the galaxy rotation curves exclude Einstein condensation in the studied galaxies.
Suppose a galaxy (not in Table 1) has a core with Einstein condensation. Let bosons in excited states fall to the ground state. The pressure will drop and hence more bosons will fall to smaller r and condense, and the process is runaway. But this condensation and collapse does not occur in the galaxies studied in this article. Einstein condensation would show up as a divergence of
as
in Figure 1.
Fits to rotation curves of galaxy NGC 3198 for several values of
are summarized in Table 5. From this Table we conclude, with 99% confidence, that
Table 5. Fits to the rotation curves of galaxy NGC 3198 for several values of
to study the onset of fermion or boson degeneracy. The four fitted parameters are
and
defined in Equation (9), and
and
. The number of degrees of freedom is 22. From this table we conclude, with 99% confidence, that
eV for fermions, and
eV for bosons. This limit for bosons sets in before Einstein condensation at
eV.
,
.
eV for fermions, and
eV for bosons, if they dominate the dark matter density. Einstein condensation sets in at
eV.
As another example let us consider galaxy NGC 2403. For fermions, degeneracy sets in at
eV, full degeneracy begins at
eV, and the limit we can set based on the increase of the
of the fit by 9 units is
eV. For bosons, degeneracy sets in at
eV, Einstein condensation begins at
eV, and for NGC 2403 no limit on
can be set based on the increase of
. Additional examples are presented in Table 4.
In conclusion, the observed spiral galaxy rotation curves disfavor dark matter dominated by axion-like bosons with mass less than 45 eV.
8. Measurement of the Dark Matter Particle Mass mh
To be specific let us consider galaxy NGC 2403. The observed rotation curves of this galaxy, presented in Figure 2, are obtained with the 4 fitted parameters listed in Table 1. In particular
km/s, and
. Derived parameters are presented in Table 3. The mean dark matter density in the sphere of proper radius
is
. We wish to relate these parameters to the primordial root-mean-square velocity of dark matter particles when perturbations were linear. We assume that dark matter particles have decoupled while still ultrarelativistic, i.e. have negligible interactions besides gravity. We take
.
A model of the hierarchical formation of galaxies is described in References [5] and [6] . Consider the expanding sphere of proper radius
and comoving radius
at time
containing the matter that will form galaxy NGC 2403. This sphere expands, reaches maximum expansion, and then collapses to form galaxy NGC 2403, see figure 5 of Reference [6] . We estimate the root-mean-square velocity of dark matter at time
, when perturbations are still linear, to be
(15)
The absolute velocity
has contributions from three spatial components, hence the factor
. The last factor is a correction corresponding to adiabatic compression. According to the model of the hierarchical formation of galaxies, Equation (15) should be valid even with merging of galaxies. A correction due to mixing, expected to be of order O(1), may be needed. Extrapolating to the past, we find that the expansion parameter at which dark matter particles become non-relativistic is
(16)
and the corresponding photon temperature is
eV. Note that
for non-relativistic particles, and the expansion parameter at time
is
. Equation (16) assumes that dark matter particles decoupled while still ultra-relativistic. To be specific, we assume that particles of mass
dominate dark matter, and that these particles have
boson degrees of freedom, and
fermion degrees of freedom. The number density of dark matter particles at expansion parameter
can be calculated in two ways:
(17)
where the ultra-relativistic expression to the right assumes zero chemical potential. Substituting
, we obtain
eV. The ratio of the temperatures of dark matter and photons is
after
annihilation while dark matter remains ultra-relativistic. Repeating these calculations for other galaxies, and including statistical uncertainties derived from the uncertainties of the measured galaxy rotation curves, we obtain Table 6.
Note that
and
drop out of the expression for
:
(18)
with
. This equation can be understood directly: it expresses
, were the last factor in (18) is the “expansion parameter” in the core of the galaxy.
Table 6. Measurements of the expansion parameter
at which dark matter becomes non-relativistic (calculated with Equation (18), and the fits in Table 1). All uncertainties are statistical, 1σ. The parameter correlation coefficient −0.802 between
and
is taken into account. Also shown are two parameters derived from
: the dark matter particle mass
, and the ratio of temperatures
of dark matter and photons after
annihilation and before dark matter becomes non-relativistic. * Galaxy NGC 2841 was excluded from the average because the measurement of
does not reach the core, see Figure 3. The uncertainty of the average is multiplied by
(as recommended in [2] ).
Alternatively, (18) expresses adiabatic expansion of a non-relativistic ideal “noble” gas:
= constant with
. By “noble” we mean that collisions (if any) between dark matter particles do not excite internal degrees of freedom (if any) of these particles.
The independent measurements of
presented in Table 6 are fairly consistent, considering that the masses
of the galaxies span three orders of magnitude, and the angular momenta
span five orders of magnitude. The average over nine independent measurements presented in Table 6 is
(19)
and the average
, after
annihilation while dark matter is still ultra-relativistic, is
(20)
where T is the photon temperature. Note that
and
, so the correlated uncertainties of
and
can be derived directly from the uncertainty of
.
The near coincidence of the two temperatures
and T is evidence that dark matter was once in thermal equilibrium with the (pre?) Standard Model particles, which explains the observed Boltzmann distribution. From the preceding analysis we also conclude that dark matter decoupled while still ultra-relativistic, so scenarios with freeze-out, or freeze-in are disfavored.
Let us summarize. We assume that ultra-relativistic dark matter has zero chemical potential, and obtain, from the spiral galaxy rotation curves, a value of
that is consistent with thermal equilibrium of dark matter with the Standard Model sector at some time in the early Universe. This is a highly significant result since T depends on
while
does not. If we would have obtained a different value of the “adiabatic invariant”
, we would have concluded that the chemical potential of dark matter is different from zero, and/or dark matter was never in thermal equilibrium with the Standard Model sector. So the observed adiabatic invariant is strong evidence that dark matter has zero chemical potential and was once in thermal equilibrium with the Standard Model particles.
9. Estimate of Systematic Uncertainties
The statistical uncertainties (at 68% confidence) presented so far are derived from the observational uncertainties of the galaxy rotation curves, and contributions from h and
.
The main systematic uncertainty comes from Equation (15). This Equation is justified by the model of the hierarchical formation of galaxies [5] [6] , and should be valid even for merging galaxies. Never-the-less Equation (15) may require a correction due to mixing. Consider galaxy NGC 3198. The time for a particle of dark matter to traverse the radius
is 1.3 Gyr, so mixing due to particles entering and leaving the sphere occupied by the galaxy may be important. At time
mixing can be neglected because the Universe is nearly homogeneous. Mixing during expansion and contraction can also be neglected. Most mixing occurs after the galaxy has formed. Even then, particles leaving and entering the sphere of proper radius
are expected to have approximately the same
, exept for a correction due to the expansion of the Universe. So we expect the correction due to mixing to be O(1) for galaxies in a stationary state, as confirmed by the fair consistency of measurements with galaxies with masses that span three orders of magnitude, and angular momenta that span five orders of magnitude. Further study of this issue is needed.
Another correction of O(1) is due to the non-spherical symmetry of the galaxies. Yet another correction of O(1) may come from the details of the transition from ultra-relativistic to non-relativistic dark matter.
Pending detailed studies, our preliminary estimates of systematic uncertainties are:
(21)
(22)
(23)
Note that (22) and (23) follow directly from (21): their uncertainties are correlated. In comparison, the current uncertainty of
spans 70 orders of magnitude for fermions, and 90 orders of magnitude for bosons [8] .
10. Thermalized Dark Matter That Decouples While Ultra-Relativistic
We consider dark matter that at some time in the history of the Universe was in thermal equilibrium with the (pre?) Standard Model particles, and decoupled from these particles and from self-annihilation while still ultra-relativistic. To be specific, we consider dark matter to be dominated by a single family of sterile Majorana neutrinos, i.e.
boson degrees of freedom, and
fermion degrees of freedom (for spin-up and spin-down). We also assume three families of active Majorana neutrinos with
each.
As the universe expands and cools, Standard Model particles and antiparticles that become non-relativistic annihilate heating the Standard Model sector conserving entropy, without heating sterile and active neutrinos if they have already decoupled. Table 7 presents the ratio
of dark matter-to-photon temperatures after
annihilation while dark matter is still ultra-relativistic. Also presented is the value of
needed to obtain the measured
. We note that the measured
(23) and measured
(22) are consistent with decoupling at temperatures higher than approximately
.
For example, assume the decoupling temperature is in the range
to
. Then
is calculated as follows:
(24)
Table 7. We consider dark matter that was once in thermal equilibrium with the (pre?) Standard Model particles and then decoupled from these particles in the indicated temperature range. We assume no self-annihilation.
is the ratio of dark matter temperature to photon temperature after
annihilation while dark matter remains ultra-relativistic.
is the mass of particles of dark matter needed to obtain the observed
. Case
,
.
These numbers can be found in the Table in Section 21.3.2 of [2] . At the time of Big Bang Nucleosynthesis (BBN), i.e.
MeV, neutrinos with, for example,
eV are still ultra-relativistic. The density of radiation at the time of BBN increases by a factor
(25)
due to one family of sterile Majorana neutrinos. Equivalently, the effective number of light neutrinos increases from
to 3.062, well within BBN experimental bounds, i.e.
[2] .
An example of a sterile neutrino dark matter candidate is presented in Figure 11. The figure was obtained by integrating the corresponding Boltzmann equation for the generation of sterile Majorana neutrinos since Electroweak Symmetry Breaking (when active Majorana neutrinos acquire a Dirac mass and therefore sterile Majorana neutrinos couple to the Standard Model). Figure 11 also shows a brief history of the Universe.
11. Dark Matter-Baryon Cross-Section
Consider a hydrogen atom, or a proton, of mass
, in a circular orbit of velocity
within the core of a galaxy. The velocity
will decay with a relative rate
due to collisions with dark matter particles with cross-section
. Taking
equal to the age of the universe,
km/s, and
(see Table 1), we obtain
(26)
Figure 11. Plotted are the number density n of photons, electrons, and dark matter particles, divided by T 3, as a function of 1/T, where T is the photon temperature. In this example, the dark matter is dominated by one Majorana sterile neutrino type (two degrees of freedom: spin up, and spin down) with
eV, produced since Electroweak Symmetry Breaking (EWSB) at
GeV. The corresponding active neutrino flavor in this example has
eV, but this value is not critical. The sterile neutrino in this example enters thermal equilibrium at
GeV, and leaves thermal contact at
GeV. The mass
eV is chosen to obtain the observed
. This solution is consistent with Big Bang Nucleosynthesis. The lifetime of this sterile neutrino is
years.
independently of
.
The mean time between collisions of a dark matter particle with baryons is
. Dark matter is not in thermal equilibrium with baryons so
is larger than the age of the universe. With data of galaxy NGC 2841 we obtain
(27)
These limits are useful for dark matter masses
below the reach of direct or indirect searches, e.g.
keV. Planed direct low mass WIMP searches with the NEWS-SNO project will reach dark matter masses ≈ 0.1 GeV [2] . No searches in the
eV range are mentioned in the Dark Matter review of Reference [2] , but ideas to reach the MeV to meV mass scales are mentioned.
12. The Core
The mean baryon density of the universe is
, while the baryon density in the core of galaxy NGC 2403 is
, so matter has collapsed by a factor
in this case. What prevented
or
from collapsing all the way to
as
? In Figures 1-10 we see no increase of
or
as
down to the first measured point at
. Why a core instead of a cusp? The four parameters
,
,
, and
can fit any core radius. So, what determines these four boundary conditions?
Possibilities to consider are Bose-Einstein of Fermi-Dirac degeneracy? (the observed galaxy rotation curves obtain
at the edge of degeneracy as shown in Section 7), dark matter or baryon crossing time?, non-spherical initial density perturbations?, angular momentum of the primordial rotation field?, dominance of baryons in the core?, ongoing collapse of the core? (however baryons are already supported by the centrifugal force as shown in Section 4), etc.
In Figures 1-10 we observe that the baryon core radius, the radius
of equal densities, and the dark matter core radius are similar, and increase in this order. We also observe that the baryon density dominates at small radii. These observations suggest that baryons radiate energy conserving angular momentum, fall to the galactic plane, acquire increasingly circular orbits, until baryons are supported by the centrifugal force with
. Thereafter baryons can fall no further. For example, a proton or hydrogen atom falling into the galaxy collides with other baryons, falls to the disk and acquires circular velocity
. Once the central gravitational potential is determined mostly by baryons, dark matter rests in this given potential.
Note that as
,
with
. Note that (18) obtains
given
and
, and therefore constrains the dark matter core radius.
13. Angular Momentum
The suggestion is that the primordial angular momentum in the sphere of proper radius
and comoving radius
during the expansion phase at time
is the same as the angular momentum
of the galaxy with
listed in Table 4, i.e. the angular momentum of the galaxy is conserved and may be of cosmological origin.
Perturbations of density, gravitational potential, and velocity in the non-relativistic universe dominated by dark matter have four independent modes [9] : a scalar growing mode, a scalar decaying mode, and two vector modes with transverse velocity (
in Fourier space) that conserve angular momentum, i.e.
. The velocity field of these vector modes is measured by the galaxy angular momenta listed in Table 4 if they are of cosmological origin.
14. Structure Formation
Most dark matter should have been non-relativistic at the time when there was a galactic mass inside the horizon [2] . From this criterion we have estimated
keV for unsuppressed formation of galaxies with total (baryonic plus dark) mass as low as
[10] . On the other hand, simulations of the Cold Dark Matter scenario produce many more dwarf galaxies than observed [11] .
At an expansion parameter
, when dark matter with mass
eV becomes non-relativistic, the universe is still dominated by radiation, see Figure 11. The age of the universe is
, the distance to the horizon is
, and the mass of baryons inside the horizon is
, comparable to large galaxies in Table 3. Smaller size perturbations are suppressed, so we may have a problem understanding the formation of galaxies with
.
Note that protons are non-relativistic when the smallest observed galaxies and globular clusters enter the horizon. Compared to the cold dark matter scenario with
keV, for
eV the power spectrum of density fluctuations on scales smaller than
becomes suppressed. If the dark matter inside the horizon becomes nearly homogeneous while ultra-relativistic (as expected), then the suppression factor is
assuming adiabatic initial conditions.
The hierarchical formation of galaxies is shown in figure 6 of Reference [6] . Suppose that only the small scale perturbations are suppressed by a factor 0.16. Since some galaxies with
have formed, other perturbations on this scale are on the verge of formation, and hence even low amplitude small scale perturbations can collapse and form a small galaxy or globular cluster. This observation may address the “missing satellite problem” [11] . A dedicated study of this issue is needed.
Dark matter with mass ≈ 69 eV also has tension with studies of the power spectra of density perturbations on scales less than 10 h−1 Mpc with the “Lyman-alpha forest” [12] . These studies set lower bounds on dark matter mass of ≈ 4 keV for early decoupled thermal relics. So we have tension between these two measurements which needs further study. Note however that 69 eV is near the limit of the reach of the Lyman-alpha forest study [12] .
15. Conclusions
We conclude that the rotation curves of regular spiral galaxies are described, within observational uncertainties, by Equations (3) to (6). These equations describe the stationary state of two self-gravitating non-relativistic ideal gases, “baryons” and “dark matter”, that do not interact significantly with each other except for gravity. These equations can be integrated numerically given four parameters (that are boundary conditions). These four parameters are obtained by minimizing a
between the measured and calculated spiral galaxy rotation curves.
From these studies, we obtain a wide range of quantitative results on the physics of galaxies, dark matter, and cosmology. In particular, we have presented precision measurements of the dark matter mass
and temperature
.
The most significant result is the ratio of the temperatures of dark matter and photons after
annihilation while dark matter is still ultra-relativistic:
(28)
The plausibility that this result is correct lies in the consistency of nine complete and independent measurements of the mass
of particles of dark matter with spiral galaxies that span three orders of magnitude in mass, and five orders of magnitude in angular momentum. The ratio (28) could have been orders of magnitude larger than, or smaller than, unity, because T depends on
, while
is independent of
. The ratio
depends on the measured adiabatic invariant
, so this analysis provides evidence that dark matter was once in thermal equilibrium with the (pre?) Standard Model particles. It is therefore likely that dark matter particles will have one of the precise masses listed in Table 7 (or in its extensions for other
or
). The decoupling of dark matter from the Standard Model sector at temperatures higher than
allows us to follow the Boltzmann distribution of these particles all the way from primordial times into the cores of spiral galaxies. An integration of the Boltzmann equation for the production of sterile Majorana neutrinos after Electroweak Symmetry Breaking shows consistency with these results, see Figure 11. Such sterile Majorana neutrinos evade all current dark matter searches.
The present studies pose new questions. Why is the spiral galaxy core radius similar in galaxies that span three orders of magnitude in mass? It seems likely that this core radius is of cosmological origin. In fact Equation (18) is already a constraint. It also seems likely that the angular momentum of spiral galaxies is of cosmological origin. Studies of angular momentum correlation between galaxies should settle this issue. If the angular momenta are cosmological, we have a handle on the amplitude of the primordial vector modes. The importance of this avenue of research lies in the fact that the velocities of these vector modes grow towards the past conserving angular momentum and hence could dominate the origin of the Universe.