<p>The dark matter has to have a <strong>roughly</strong> spherical distribution and a smooth radial distribution if it is to account for the dynamics of gas and stars in our and other Galaxies.</p>

<p>The exact shape of any required dark matter halo is still the subject of debate and research. Whilst computer simulations of galaxy formation predict mildly non-spherical or triaxial profiles (e.g. <a href="https://arxiv.org/abs/1809.07255" rel="nofollow noreferrer">Kunting et al. 2018</a>) and some stellar kinematic data appear to confirm sphericity (e.g. <a href="https://arxiv.org/abs/0902.2709" rel="nofollow noreferrer">Smith et al. 2009</a> ); others disagree and suggest there is some significant prolateness ( <a href="https://arxiv.org/abs/1604.06885" rel="nofollow noreferrer">Bowden et al. 2016</a>) or oblateness suggested by large scale surveys (e.g. <a href="https://arxiv.org/abs/1408.5388" rel="nofollow noreferrer">Loebman et al. 2014</a>).</p>

<p>Any concentration of dark matter into a disk is <strong>totally ruled out</strong> by observations of the dynamics of stars above and below the plane.
e.g. The latest word, using Gaia DR2 data, is that there can only be about 10% of the <em>local</em> mass density in the form of dark matter of any kind (<a href="https://arxiv.org/abs/1808.05603" rel="nofollow noreferrer">Buch et al. 2019</a>, agreeing with lots of previous work. For instance this was established fact at least 30 years ago (<a href="http://adsabs.harvard.edu/abs/1989MNRAS.239..651K" rel="nofollow noreferrer">Kuijken &amp; Gilmore 1989</a>).</p>

<p>The amount of dark matter required at different radii (assuming Newtonian gravity is the correct formulation)  is deduced from the rotation curve. The image below, courtesy of Nick Strobel at www.astronomynotes.com, shows a sketch of the current thinking on how much dark matter needs to be at what radius (labelled as "Corona") and takes the dark matter to be distributed spherically symmetrically.</p>

<p>Dark matter already "outweighs" luminous matter by 2:1 at the solar radius, yet there is room for only 10% of the local density to be in a "dark" form of any kind. </p>

<p><a href="https://i.sstatic.net/UCrsA.gif" rel="nofollow noreferrer"><img src="https://i.sstatic.net/UCrsA.gif" alt="Distribution of dark matter"></a></p>

<p>Brown dwarfs are not actually "dark objects" that cannot be found. They emit infrared light and surveys near the Sun reveal that stars outnumber them by 4:1 and that they contribute less than a few percent the local mass density.
They can also be found via gravitational microlensing, in surveys that have been performed towards the Magellanic clouds (sampling the halo) and towards the Galactic bulge (sampling the inner disk). In neither case has evidence been found for huge numbers of brown dwarfs (or cold white dwarfs or black holes) and these have been ruled out as significant contributors to the Galactic dark matter problem (e.g. <a href="https://www.nature.com/articles/d41586-018-07006-8" rel="nofollow noreferrer">Pietrzynski 2018</a>). In particular, the numbers of microlensing events towards the Galactic bulge is perfectly consistent with the brown dwarf/star fraction in the local neighborhood (<a href="https://arxiv.org/abs/1901.07120" rel="nofollow noreferrer">Niikura et al. (2019)</a>.</p>

<p>As a final remark, dark matter (whether in the form of brown dwarfs or non-baryonic particles) doesn't clump very easily because it cannot readily dissipate it's kinetic energy. There is little evidence for any clumping of dark matter on scales smaller than dwarf galaxies. In particular no evidence for dark matter is found in globular or open clusters of stars.</p>

<p>The stellar disk forms because the stars formed more-or-less in a disk that had already formed from dissipative baryonic gas that had already collapsed into a disk.  As brown dwarfs must also form from baryonic gas then there are really only two alternatives for their distribution. Either they follow the disk and should be associated with disk stars or they should be very old and associated with halo stars that formed in a spherical gas cloud before it collapsed to form a disk and therefore still have a spherical distribution.</p>

<p>The dark matter needs to be much more extended than the luminous matter of the Galaxy. In neither scenario described above do we end up with tens of trillions of brown dwarfs (for that is what would be required) distributed a long way outside the solar circle and unassociated with any luminous matter.</p>

CC BY-SA 4.0
2019-04-14T15:13:15.703Z
Um. I see the assertion that the dark matter is distributed spherically. What I want is some sort of computer modelling to back it. Best as I recall the models have the matter ending up in a disk. Not seen one where the dark matter is distributed differently.
Blame
CC BY-SA 4.0
2019-04-14T15:19:29.463Z
There is one argument for clumping. Dark matter seems to be associated with the ordinary stuff which clumps. If it is to stay associated then it to must clump.
Blame
CC BY-SA 4.0
2019-04-14T15:29:31.257Z
@blame All dark matter galaxy halo models are pseudospherical in shape. e.g. https://en.m.wikipedia.org/wiki/Navarro–Frenk–White_profile The dark matter doesn't follow the luminous matter because there is  10 times as much dark matter and it is dissipationless.
ProfRob
CC BY-SA 4.0
2019-04-14T15:32:17.037Z
I have given you a paper that shows there is hardly any dark matter in the disk. @blame
ProfRob
CC BY-SA 4.0
2019-04-14T16:22:45.370Z
Hmm. Ok. Clearly I have to be a lot brighter to understand that paper but it addresses the issue even if I can't quite grasp the conclusion. I think it says the dark matter probably isn't a disk...although just how much not so depends on what sort of star you ask so something is going on that they ain't sure about.
Blame
CC BY-SA 4.0
2019-04-14T19:45:18.227Z
Still would like to know about any computer modelling The evidence may say spherical but I am still confused as to how it came about. I am assuming the DM arrived with the various smaller galaxies, clusters and gas clouds from which our galaxy was formed. Just can't visualise how that results in a sphere. To be stable it just has to rotate and I would expect it to hold on to the same general direction of rotation as the stuff it came with.
Blame
CC BY-SA 4.0
2019-04-14T20:58:56.797Z
@Blame the key thing to understand is that, as far as we can tell, the Dark matter particles don't interact with anything, *including each other* except via gravity. So while gas arriving with orbits at different angles will eventually settle into a single disk oriented according to the overall angular momentum, each DM particle will just keep orbiting at whatever angle it happened to arrive at. Since those angles are fairly random, the DM ends up pretty uniformly distribute around the galactic centre of mass.
Steve Linton
CC BY-SA 4.0
2019-04-15T01:59:16.140Z
@Steve Ok. Got that. Dark matter interacts only through gravity. So not like gas. However, very much like stars?  So if the DM arrived already formed as brown dwarfs Would it be in a different location now than where we would expect particle DM?
Blame
CC BY-SA 4.0
2019-04-15T11:25:03.493Z
So.. perhaps a survey of very old stars might give a clue. They presumably arrived fully formed and thus are likely to follow something of the same distribution as DM.
Blame
CC BY-SA 4.0
2019-04-15T12:24:16.450Z
@Blame The oldest  stars are distributed in a  spherical halo - as I say above. They follow the initial distribution of gas. Gas falls into the gravitational potential well formed by dark matter.
ProfRob
CC BY-SA 4.0
2019-04-14T14:47:39.857Z
2019-04-15T12:50:31.803Z
2019-04-15T12:50:31.803Z
ProfRob
<p>We have been repeatedly assured that their ain't enough brown dwarfs to account for all the dark matter in our galaxy.</p>

<p>My question is have we been looking in the right places?</p>

<p>Or in more detail. Where exactly does computer modelling put the missing mass? </p>

<p>I would expect the bulk of it to be on the galaxy's plain and on the edge. And if I am not mistaken there is too much junk in the way to look.</p>

<p>Further I can't see any reason why the dark matter won't be unevenly distributed in clumps just like everything else. </p>

<p>So, given the above an extrapolation from what we have detected will be way low if it assumes an even distribution in all directions, and horribly low if the LMG and GMG happen to be between clumps. </p>

CC BY-SA 4.0
2019-04-14T15:25:54.177Z
Related: https://astronomy.stackexchange.com/questions/8172/what-are-the-arguments-against-the-feng-and-gallo-thin-disk-explanation-of-galac
ProfRob
CC BY-SA 4.0
2019-04-14T20:08:02.323Z
https://en.wikipedia.org/wiki/Navarro–Frenk–White_profile For some reason the entire link won't highlight.
ProfRob
<dark-matter><brown-dwarf>
Are we looking for brown dwarfs where the dark matter has to be?
Blame
# Are we looking for brown dwarfs where the dark matter has to be?

(Asked by: username_0 on 2019-04-14)

We have been repeatedly assured that their ain't enough brown dwarfs to account for all the dark matter in our galaxy.

My question is have we been looking in the right places?

Or in more detail. Where exactly does computer modelling put the missing mass?

I would expect the bulk of it to be on the galaxy's plain and on the edge. And if I am not mistaken there is too much junk in the way to look.

Further I can't see any reason why the dark matter won't be unevenly distributed in clumps just like everything else.

So, given the above an extrapolation from what we have detected will be way low if it assumes an even distribution in all directions, and horribly low if the LMG and GMG happen to be between clumps.

**Tags:** dark-matter, brown-dwarf
> **Comments:**
> **username_1**: Related: https://astronomy.stackexchange.com/questions/8172/what-are-the-arguments-against-the-feng-and-gallo-thin-disk-explanation-of-galac  
> **username_1**: https://en.wikipedia.org/wiki/Navarro–Frenk–White_profile For some reason the entire link won't highlight.  

---

## 1 answers

### Answer by username_1 on 2019-04-14. Score: 6

The dark matter has to have a **roughly** spherical distribution and a smooth radial distribution if it is to account for the dynamics of gas and stars in our and other Galaxies.

The exact shape of any required dark matter halo is still the subject of debate and research. Whilst computer simulations of galaxy formation predict mildly non-spherical or triaxial profiles (e.g. [Kunting et al. 2018](https://arxiv.org/abs/1809.07255)) and some stellar kinematic data appear to confirm sphericity (e.g. [Smith et al. 2009](https://arxiv.org/abs/0902.2709) ); others disagree and suggest there is some significant prolateness ( [Bowden et al. 2016](https://arxiv.org/abs/1604.06885)) or oblateness suggested by large scale surveys (e.g. [Loebman et al. 2014](https://arxiv.org/abs/1408.5388)).

Any concentration of dark matter into a disk is **totally ruled out** by observations of the dynamics of stars above and below the plane.
e.g. The latest word, using Gaia DR2 data, is that there can only be about 10% of the *local* mass density in the form of dark matter of any kind ([Buch et al. 2019](https://arxiv.org/abs/1808.05603), agreeing with lots of previous work. For instance this was established fact at least 30 years ago ([Kuijken & Gilmore 1989](http://adsabs.harvard.edu/abs/1989MNRAS.239..651K)).

The amount of dark matter required at different radii (assuming Newtonian gravity is the correct formulation) is deduced from the rotation curve. The image below, courtesy of Nick Strobel at www.astronomynotes.com, shows a sketch of the current thinking on how much dark matter needs to be at what radius (labelled as "Corona") and takes the dark matter to be distributed spherically symmetrically.

Dark matter already "outweighs" luminous matter by 2:1 at the solar radius, yet there is room for only 10% of the local density to be in a "dark" form of any kind.

[![Distribution of dark matter](https://i.sstatic.net/UCrsA.gif)](https://i.sstatic.net/UCrsA.gif)

Brown dwarfs are not actually "dark objects" that cannot be found. They emit infrared light and surveys near the Sun reveal that stars outnumber them by 4:1 and that they contribute less than a few percent the local mass density.
They can also be found via gravitational microlensing, in surveys that have been performed towards the Magellanic clouds (sampling the halo) and towards the Galactic bulge (sampling the inner disk). In neither case has evidence been found for huge numbers of brown dwarfs (or cold white dwarfs or black holes) and these have been ruled out as significant contributors to the Galactic dark matter problem (e.g. [Pietrzynski 2018](https://www.nature.com/articles/d41586-018-07006-8)). In particular, the numbers of microlensing events towards the Galactic bulge is perfectly consistent with the brown dwarf/star fraction in the local neighborhood ([Niikura et al. (2019)](https://arxiv.org/abs/1901.07120).

As a final remark, dark matter (whether in the form of brown dwarfs or non-baryonic particles) doesn't clump very easily because it cannot readily dissipate it's kinetic energy. There is little evidence for any clumping of dark matter on scales smaller than dwarf galaxies. In particular no evidence for dark matter is found in globular or open clusters of stars.

The stellar disk forms because the stars formed more-or-less in a disk that had already formed from dissipative baryonic gas that had already collapsed into a disk. As brown dwarfs must also form from baryonic gas then there are really only two alternatives for their distribution. Either they follow the disk and should be associated with disk stars or they should be very old and associated with halo stars that formed in a spherical gas cloud before it collapsed to form a disk and therefore still have a spherical distribution.

The dark matter needs to be much more extended than the luminous matter of the Galaxy. In neither scenario described above do we end up with tens of trillions of brown dwarfs (for that is what would be required) distributed a long way outside the solar circle and unassociated with any luminous matter.

> **Comments:**
> **username_0**: Um. I see the assertion that the dark matter is distributed spherically. What I want is some sort of computer modelling to back it. Best as I recall the models have the matter ending up in a disk. Not seen one where the dark matter is distributed differently.  
> **username_0**: There is one argument for clumping. Dark matter seems to be associated with the ordinary stuff which clumps. If it is to stay associated then it to must clump.  
> **username_1**: @blame All dark matter galaxy halo models are pseudospherical in shape. e.g. https://en.m.wikipedia.org/wiki/Navarro–Frenk–White_profile The dark matter doesn't follow the luminous matter because there is  10 times as much dark matter and it is dissipationless.  
> **username_1**: I have given you a paper that shows there is hardly any dark matter in the disk. @blame  
> **username_0**: Hmm. Ok. Clearly I have to be a lot brighter to understand that paper but it addresses the issue even if I can't quite grasp the conclusion. I think it says the dark matter probably isn't a disk...although just how much not so depends on what sort of star you ask so something is going on that they ain't sure about.  
> **username_0**: Still would like to know about any computer modelling The evidence may say spherical but I am still confused as to how it came about. I am assuming the DM arrived with the various smaller galaxies, clusters and gas clouds from which our galaxy was formed. Just can't visualise how that results in a sphere. To be stable it just has to rotate and I would expect it to hold on to the same general direction of rotation as the stuff it came with.  
> **username_2**: @Blame the key thing to understand is that, as far as we can tell, the Dark matter particles don't interact with anything, *including each other* except via gravity. So while gas arriving with orbits at different angles will eventually settle into a single disk oriented according to the overall angular momentum, each DM particle will just keep orbiting at whatever angle it happened to arrive at. Since those angles are fairly random, the DM ends up pretty uniformly distribute around the galactic centre of mass.  
> **username_0**: @Steve Ok. Got that. Dark matter interacts only through gravity. So not like gas. However, very much like stars?  So if the DM arrived already formed as brown dwarfs Would it be in a different location now than where we would expect particle DM?  
> **username_0**: So.. perhaps a survey of very old stars might give a clue. They presumably arrived fully formed and thus are likely to follow something of the same distribution as DM.  
> **username_1**: @Blame The oldest  stars are distributed in a  spherical halo - as I say above. They follow the initial distribution of gas. Gas falls into the gravitational potential well formed by dark matter.  

---

