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## Density of the inter-cluster medium

 Quote by SpaceTiger Well, firstly, I don't think there's any reason that all of the gas in an overdensity should have to collapse into galaxies (note that there is still material falling in from outside of clusters).
That is interesting ST. How dense is the inter-galactic-cluster medium?
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 Quote by Garth That is interesting ST. How dense is the inter-galactic-cluster medium?
This is a great question Garth ... and if I may add a rider: and how is such density measured/inferred?

If you don't mind, I'd like to keep this thread to just QSO absorption lines (and closely related topics) - May I split this off as the start of a new thread?

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 Quote by Nereid But first, for those not quite in the know, what is the "WHIM"?
WHIM stands for Warm-Hot Intergalactic Medium, a low density phase at 105 - 107 K, mainly located in the filaments and not part of any virialized system. About 30% - 40% of all baryons of the present universe (z < 2) were assumed to reside in this phase. It was postulated here and there is some observational evidence in the meanwhile.

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## Density of the inter-cluster medium

 Quote by Garth That is interesting ST. How dense is the inter-galactic-cluster medium?
There are two main components to the intergalactic medium, the cold component (T<105 K) and the warm-hot component (105-107 K). The former is only a few times the critical density:

$$\rho_c=\frac{3H^2}{8\pi G}$$

corresponding to a density of about 10-5 cm-3. The warm-hot component is about a factor of ten more dense than this. Finally, intracluster gas has densities of order 10-3 cm-3 and temperatures of around 107 K.

You can determine these conditions from a lot of things, including fitting absorption lines in quasar spectra, looking at X-ray emission and absorption, and the Sunyaev-Zeldovich effect.

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 Quote by SpaceTiger There are two main components to the intergalactic medium, the cold component (T<105 K) and the warm-hot component (105-107 K). The former is only a few times the critical density: $$\rho_c=\frac{3H^2}{8\pi G}$$ corresponding to a density of about 10-5 cm-3. The warm-hot component is about a factor of ten more dense than this. Finally, intracluster gas has densities of order 10-3 cm-3 and temperatures of around 107 K. You can determine these conditions from a lot of things, including fitting absorption lines in quasar spectra, looking at X-ray emission and absorption, and the Sunyaev-Zeldovich effect.
These densities seem very high ST - with the critical density at around 10-29 cm-3?

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 Quote by Garth These densities seem very high ST - with the critical density at around 10-29 cm-3?
That's 10-29 g cm-3. I was quoting densities in terms of atoms per unit volume (instead of mass per unit volume).

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