<p>We know that most of the matter in the universe has collapsed into galaxies and galaxies into groups and clusters and that a lot of matter is presently in clusters between the galaxies.  But, what fraction of total matter is not represented by these discrete observed entities?  Some dark matter may have velocities too high to fall into halos perhaps from tidal tails that escape mergers.  There must be some relic medium in voids with a density too low to form galaxies.  Some halos may be too small to form stars.  Does all of this add up to a significant intergalactic medium (IGM)?  Do n-body simulations give a number for this?</p>
<p>One might think that we could get the answer to this question by adding up all the known mass in the nearby universe and subtracting it from the CMB derived mean density of the universe times the volume used.  But some recent observational studies are suggesting that the local density is well below the mean density and that this is the cause of the Hubble Constant discrepancy.</p>

CC BY-SA 4.0
2021-03-27T11:00:22.237Z
The IGM is very sparse, but the volume is vast.
PM 2Ring
CC BY-SA 4.0
2021-03-30T12:56:20.307Z
Do you consider sheets and filaments to be a collapsed entity. If so, there's only voids left, and then I agree that most matter has collapsed. But if you only consider collapsed matter up until clusters, then I think it's not true that most matter has collapsed.
pela
CC BY-SA 4.0
2021-03-30T17:23:29.097Z
I would include all matter that is not lit up and thus not included in a tally of mass from applying a mass-to-light ratio to galaxies or applying the virial theorem to clusters and groups.  So sheets and filaments, but not the lit up knots in them, would be included since they are dark.
eshaya
<dark-matter><n-body-simulations><intergalactic-space>
What fraction of matter is not bound to the galaxies, groups and clusters that we see?
eshaya
# What fraction of matter is not bound to the galaxies, groups and clusters that we see?

(Asked by: username_0 on 2021-03-27)

We know that most of the matter in the universe has collapsed into galaxies and galaxies into groups and clusters and that a lot of matter is presently in clusters between the galaxies. But, what fraction of total matter is not represented by these discrete observed entities? Some dark matter may have velocities too high to fall into halos perhaps from tidal tails that escape mergers. There must be some relic medium in voids with a density too low to form galaxies. Some halos may be too small to form stars. Does all of this add up to a significant intergalactic medium (IGM)? Do n-body simulations give a number for this?

One might think that we could get the answer to this question by adding up all the known mass in the nearby universe and subtracting it from the CMB derived mean density of the universe times the volume used. But some recent observational studies are suggesting that the local density is well below the mean density and that this is the cause of the Hubble Constant discrepancy.

**Tags:** dark-matter, n-body-simulations, intergalactic-space
> **Comments:**
> **username_1**: The IGM is very sparse, but the volume is vast.  
> **username_2**: Do you consider sheets and filaments to be a collapsed entity. If so, there's only voids left, and then I agree that most matter has collapsed. But if you only consider collapsed matter up until clusters, then I think it's not true that most matter has collapsed.  
> **username_0**: I would include all matter that is not lit up and thus not included in a tally of mass from applying a mass-to-light ratio to galaxies or applying the virial theorem to clusters and groups.  So sheets and filaments, but not the lit up knots in them, would be included since they are dark.  

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## 0 answers

