The Interstellar Medium

or "the stuff between the stars"

Interstellar space is not empty -- there is lots of gas and dust in the galaxy. Dust we talked about -- its presence causes an extinction and reddening of starlight that passes through it. What about this gas stuff?

The chemical composition of the gas is mostly hydrogen (~70%), a little bit of metals (~ few %) and the rest helium. What does this sound like?

Depending on the physical conditions around the gas, it can be either

mixed with the helium and metals, of course... How do we see this gas? Because it is diffuse, it does not act like a blackbody, so we don't see a continuous spectrum (like stars).


 
Ionized hydrogen ("HII regions")
Near hot stars, the intense UV light can ionize the hydrogen atoms. When the electrons and protons recombine, they generally recombine to upper energy levels (large n), and then cascade down, emitting Balmer lines. Then they can be reionized, and the cycle continues. So we see Balmer emission lines, as well as lines from other atoms (ie oxygen, sulfer, silicon, carbon...).

These HII regions are associated with regions of active star formation. Why do we know there are young stars there?


(From Schweizer et al 2013)


In galaxies, HII regions trace star formation

Left: M101 B image showing stars (Mihos et al 2013), Right: M101 Hα\alpha image showing star forming regions (Watkins et al in prep):



Neutral hydrogen (HI)

Far away from stars, there is nothing to ionize the gas, or even excite the electrons to higher energy levels. The hydrogen is in the ground state (n=1), so there are no downward transitions to make emission lines. How then can we see this gas?
Atomic physics: particles have angular momentum (spin, described by the quantum number m). Because they have charge, and are spinning, they act sort of like little magnets. The electron and proton want to be anti-aligned so that they have opposite spin -- this is their ground state. If they are aligned, they have slightly more energy; they can change their spin and release this energy difference as a photon.

The energy difference is small - about 6x10-6 eV. This corresponds to a wavelength of 21 cm -- radio waves!
 

How often does this happen? For a given atom, about once every several million years. But if you have enough atoms...

What happens if we look at M101 in 21-cm radio emission? 

Left: M101 B image showing stars (Mihos et al 2013), Right: M101 21-cm image showing neutral hydrogen (THINGS team):   


So there's lots of gas out there. In our galaxy, there is about 1 solar mass of gas for every 10 solar masses of stars.



Molecular gas
If the density of the gas is high, and the temperature is cold enough, hydrogen atoms can form molecular hydrogen (H2). Unfortunately, there is no emission from H2 in the optical or radio bands -- it is very hard to observe. How can we see it?

1. Look at other molecules (where you have one molecule, you'll probably have others). For example, CO emits radiation at a wavelength of 2.6mm -- microwaves!

Look at the nearby galaxy M51:

2. Look for dust. Dust and molecules are often found together (why?) Dense, dark clouds (called Bok globules) are regions of very dense molecular gas.

Where we see lots of gas -- in particular molecular gas and ionized gas -- we see lots of stars forming...